FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Chekhtman, A
Chen, AW
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Colafrancesco, S
Conrad, J
Cutini, S
Dermer, CD
de Palma, F
Digel, SW
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Farnier, C
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Frailis, M
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grandi, P
Grenier, IA
Guillemot, L
Guiriec, S
Hadasch, D
Harding, AK
Hayashida, M
Horan, D
Hughes, RE
Itoh, R
Jackson, MS
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Kawai, N
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Makeev, A
Mazziotta, MN
McEnery, JE
McGlynn, S
Meurer, C
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nestoras, I
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reyes, LC
Rodriguez, AY
Roth, M
Ryde, F
Sadrozinski, HFW
Sambruna, R
Sander, A
Sato, R
Sgro, C
Shaw, MS
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Stawarz, L
Stecker, FW
Strickman, MS
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibolla, O
Torres, DF
Tosti, G
Tramacere, A
Uchiyama, Y
Usher, TL
Vasileiou, V
Vilchez, N
Villata, M
Vitale, V
von Kienlin, A
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
Tavecchio, F
Sikora, M
Schady, P
Roming, P
Chester, MM
Maraschi, L
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Chekhtman, A.
Chen, A. W.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Colafrancesco, S.
Conrad, J.
Cutini, S.
Dermer, C. D.
de Palma, F.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Farnier, C.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Frailis, M.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grandi, P.
Grenier, I. A.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Hayashida, M.
Horan, D.
Hughes, R. E.
Itoh, R.
Jackson, M. S.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kawai, N.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Makeev, A.
Mazziotta, M. N.
McEnery, J. E.
McGlynn, S.
Meurer, C.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nestoras, I.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reyes, L. C.
Rodriguez, A. Y.
Roth, M.
Ryde, F.
Sadrozinski, H. F. -W.
Sambruna, R.
Sander, A.
Sato, R.
Sgro, C.
Shaw, M. S.
Siskind, E. J.
Smith, P. D.
Spandre, G.
Spinelli, P.
Stawarz, L.
Stecker, F. W.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibolla, O.
Torres, D. F.
Tosti, G.
Tramacere, A.
Uchiyama, Y.
Usher, T. L.
Vasileiou, V.
Vilchez, N.
Villata, M.
Vitale, V.
von Kienlin, A.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
Tavecchio, F.
Sikora, M.
Schady, P.
Roming, P.
Chester, M. M.
Maraschi, L.
TI SUZAKU OBSERVATIONS OF LUMINOUS QUASARS: REVEALING THE NATURE OF
HIGH-ENERGY BLAZAR EMISSION IN LOW-LEVEL ACTIVITY STATES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; radiation mechanisms: non-thermal;
X-rays: galaxies
ID XMM-NEWTON OBSERVATIONS; MAGNETOSONIC SHOCK-WAVES; LARGE-AREA TELESCOPE;
RADIO-LOUD QUASARS; X-RAY TELESCOPE; MULTIWAVELENGTH OBSERVATIONS;
GALACTIC NUCLEI; 3C 454.3; AMBIENT RADIATION; NONTHERMAL FLARES
AB We present the results from the Suzaku X-ray observations of five flat-spectrum radio quasars (FSRQs), namely PKS 0208-512, Q 0827+243, PKS 1127-145, PKS 1510-089, and 3C 454.3. All these sources were additionally monitored simultaneously or quasi-simultaneously by the Fermi satellite in gamma rays and the Swift UVOT in the UV and optical bands, respectively. We constructed their broadband spectra covering the frequency range from 10(14) Hz up to 10(25) Hz, and those reveal the nature of high-energy emission of luminous blazars in their low-activity states. The analyzed X-ray spectra are well fitted by a power-law model with photoelectric absorption. In the case of PKS 0208-512, PKS 1127-145, and 3C 454.3, the X-ray continuum showed indication of hardening at low energies. Moreover, when compared with the previous X-ray observations, we see a significantly increasing contribution of low-energy photons to the total X-ray fluxes when the sources are getting fainter. The same behavior can be noted in the Suzaku data alone. A likely explanation involves a variable, flat-spectrum component produced via inverse-Compton emission, plus an additional, possibly steady soft X-ray component prominent when the source gets fainter. This soft X-ray excess is represented either by a steep power-law (photon indices Gamma similar to 3-5) or a blackbody-type emission with temperatures kT similar to 0.1-0.2 keV. We model the broadband spectra of the five observed FSRQs using synchrotron self-Compton and/or external-Compton radiation models. Our modeling suggests that the difference between the low-and high-activity states in luminous blazars is due to the different total kinetic power of the jet, most likely related to varying bulk Lorentz factor of the outflow within the blazar emission zone.
C1 [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; 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.] Univ Paris Diderot, Lab AIM, CNRS, CEA IRFU,Serv Astrophys,CEA Saclay, 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, Dipartimento Fis, I-34127 Trieste, Italy.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Carrigan, S.; Rando, R.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Brigida, M.; 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.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Cavazzuti, E.; Colafrancesco, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[Celik, Oe.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; McEnery, J. E.; Sambruna, R.; Stecker, F. W.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Chen, A. W.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Conrad, J.; Meurer, C.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Jackson, M. S.; McGlynn, S.; Meurer, C.; Ryde, F.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dumora, D.; Guillemot, L.; Lott, B.; Parent, D.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France.
[Dumora, D.; Guillemot, L.; Lott, B.; Parent, D.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Frailis, M.; Roming, P.; Chester, M. M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Grandi, P.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Guillemot, L.; Nestoras, I.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Hadasch, D.; Torres, D. F.] ICREA, Barcelona, Spain.
[Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Jackson, M. S.; McGlynn, S.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan.
[Kawai, N.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[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.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Orlando, E.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ozaki, M.; Sato, R.; Stawarz, L.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Reyes, L. C.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reyes, L. C.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Sadrozinski, H. F. -W.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Tramacere, A.; Tavecchio, F.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, 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.
[Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Schady, P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Maraschi, L.] Osservatorio Astron Brena, I-20121 Milan, Italy.
[Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden.
RP Abdo, AA (reprint author), USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
EM rsato@astro.isas.jaxa.jp
RI Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Ozaki,
Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; 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; Johnson,
Neil/G-3309-2014; XRAY, SUZAKU/A-1808-2009; 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 Reimer, Olaf/0000-0001-6953-1385; Thompson, David/0000-0001-5217-9135;
lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888;
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; Sgro',
Carmelo/0000-0001-5676-6214; Villata, Massimo/0000-0003-1743-6946;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; giommi, paolo/0000-0002-2265-5003;
Frailis, Marco/0000-0002-7400-2135; Grandi, Paola/0000-0003-1848-6013;
Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Giroletti, Marcello/0000-0002-8657-8852;
Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X;
Gasparrini, Dario/0000-0002-5064-9495; Tramacere,
Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie 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; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie 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.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.; L. S. was
partially supported by the Polish Ministry of Science and Higher
Education through the project N N203 380336.
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SC Astronomy & Astrophysics
GA 600CD
UT WOS:000277960000064
ER
PT J
AU Lichtenberg, KA
Arvidson, RE
Morris, RV
Murchie, SL
Bishop, JL
Remolar, DF
Glotch, TD
Dobrea, EN
Mustard, JF
Andrews-Hanna, J
Roach, LH
AF Lichtenberg, Kimberly A.
Arvidson, Raymond E.
Morris, Richard V.
Murchie, Scott L.
Bishop, Janice L.
Fernandez Remolar, David
Glotch, Timothy D.
Dobrea, Eldar Noe
Mustard, John F.
Andrews-Hanna, Jeffrey
Roach, Leah H.
TI Stratigraphy of hydrated sulfates in the sedimentary deposits of Aram
Chaos, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MERIDIANI-PLANUM; OMEGA/MARS EXPRESS
AB Sedimentary deposits within the 280 km wide crater containing Aram Chaos (similar to 3 degrees N, 339 degrees E) have been differentially eroded by wind to expose a stratigraphic column 900-1000 m thick that unconformably overlies the chaos bedrock. A detailed stratigraphic and mineralogical description of the deposits is presented based on data from the Mars Reconnaissance Orbiter Compact Reconnaissance Imaging Spectrometer for Mars, Context Imager, and High Resolution Imaging Science Experiment. Two sedimentary units overlie the basement chaos material representing the original plains fill in Aram Crater: the first and oldest is composed of (1) a 50-75 m thick dark-toned basal unit containing ferric hydroxysulfate intercalated with monohydrated-sulfate-bearing materials, (2) a 75-100 m thick light-toned unit with monohydrated sulfates, and (3) a 175-350 m thick light-toned resistant capping unit with nanophase ferric oxides and monohydrated sulfates. After a period of wind erosion, these deposits were partially and unconformably covered by the second sedimentary unit, a 75-100 m thick, discontinuous dark-toned unit containing crystalline hematite and polyhydrated sulfate material. These sedimentary deposits were formed by evaporite deposition during at least two distinct rising groundwater episodes fed by regional-scale recharge. Later groundwater event(s) formed the polyhydrated materials, indicating that environmental conditions changed to a higher water-to-rock ratio. Wind has continued to shape the landscape after the last wetting event to produce the features and exposures observed.
C1 [Lichtenberg, Kimberly A.; Arvidson, Raymond E.] Washington Univ, McDonnell Ctr Space Sci, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Andrews-Hanna, Jeffrey] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA.
[Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA.
[Fernandez Remolar, David] INTA CSIC, Ctr Astrobiol, E-28850 Madrid, Spain.
[Glotch, Timothy D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Morris, Richard V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Mustard, John F.; Roach, Leah H.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Dobrea, Eldar Noe] Planetary Sci Inst, Tucson, AZ 85719 USA.
RP Lichtenberg, KA (reprint author), Washington Univ, McDonnell Ctr Space Sci, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
EM lichtenberg@wunder.wustl.edu
RI Murchie, Scott/E-8030-2015
OI Murchie, Scott/0000-0002-1616-8751
FU NASA; Micinn Project [ESP2006-09487]
FX K. A. Lichtenberg, R. E. Arvidson, and R. V. Morris acknowledge support
from NASA for participation as CRISM Science Team Members. We thank J.
Gruener (NASA-JSC) for the XRD powder patterns of the synthetic
sulfate-bearing phases. David Fernandez-Remolar acknowledges support by
the Micinn Project ESP2006-09487. We would also like to thank our two
reviewers for the thoughtful and thorough comments which made this a
better paper.
NR 40
TC 46
Z9 48
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 JUN 10
PY 2010
VL 115
AR E00D17
DI 10.1029/2009JE003353
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 610MC
UT WOS:000278735900001
ER
PT J
AU Boykin, PO
Mor, T
Roychowdhury, V
Vatan, F
AF Boykin, P. Oscar
Mor, Tal
Roychowdhury, Vwani
Vatan, Farrokh
TI Algorithms on ensemble quantum computers
SO NATURAL COMPUTING
LA English
DT Article; Proceedings Paper
CT 6th International Conference on Unconventional Computation
CY AUG, 2007
CL Kingston, CANADA
SP EATCS, Cent Discrete Math & Theoret Comp Sci, Queens Univ, Sch Comp
DE Quantum algorithms; Ensemble (bulk) quantum computers; NMR; Fault
tolerance computing
ID NUCLEAR-MAGNETIC-RESONANCE; ERROR-CORRECTION; COMPUTATION;
TELEPORTATION; SPINS
AB In ensemble (or bulk) quantum computation, all computations are performed on an ensemble of computers rather than on a single computer. Measurements of qubits in an individual computer cannot be performed; instead, only expectation values (over the complete ensemble of computers) can be measured. As a result of this limitation on the model of computation, many algorithms cannot be processed directly on such computers, and must be modified, as the common strategy of delaying the measurements usually does not resolve this ensemble-measurement problem. Here we present several new strategies for resolving this problem. Based on these strategies we provide new versions of some of the most important quantum algorithms, versions that are suitable for implementing on ensemble quantum computers, e. g., on liquid NMR quantum computers. These algorithms are Shor's factorization algorithm, Grover's search algorithm (with several marked items), and an algorithm for quantum fault-tolerant computation. The first two algorithms are simply modified using a randomizing and a sorting strategies. For the last algorithm, we develop a classical-quantum hybrid strategy for removing measurements. We use it to present a novel quantum fault-tolerant scheme. More explicitly, we present schemes for fault-tolerant measurement-free implementation of Toffoli and sigma(1/4)(z) as these operations cannot be implemented "bitwise", and their standard fault-tolerant implementations require measurement.
C1 [Mor, Tal] Technion, Dept Comp Sci, IL-32000 Haifa, Israel.
[Boykin, P. Oscar] Univ Florida, Dept Elect & Comp Engn, Gainesville, FL 32611 USA.
[Roychowdhury, Vwani] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Vatan, Farrokh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mor, T (reprint author), Technion, Dept Comp Sci, IL-32000 Haifa, Israel.
EM talmo@cs.technion.ac.il
NR 27
TC 4
Z9 4
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1567-7818
EI 1572-9796
J9 NAT COMPUT
JI Nat. Comput.
PD JUN 10
PY 2010
VL 9
IS 2
BP 329
EP 345
DI 10.1007/s11047-009-9133-0
PG 17
WC Computer Science, Artificial Intelligence; Computer Science,
Interdisciplinary Applications; Computer Science, Theory & Methods
SC Computer Science
GA 604GK
UT WOS:000278267300004
ER
PT J
AU Zaitchik, BF
Rodell, M
Olivera, F
AF Zaitchik, Benjamin F.
Rodell, Matthew
Olivera, Francisco
TI Evaluation of the Global Land Data Assimilation System using global
river discharge data and a source-to-sink routing scheme
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; SURFACE MODEL; CONTINENTAL-SCALE;
PRECIPITATION PRODUCTS; TEMPORAL ANALYSIS; BASIN EXPERIMENT; CLIMATE
MODELS; SNOW COVER; PARAMETERIZATION; RUNOFF
AB Advanced land surface models (LSMs) offer detailed estimates of distributed hydrological fluxes and storages. These estimates are extremely valuable for studies of climate and water resources, but they are difficult to verify as field measurements of soil moisture, evapotranspiration, and surface and subsurface runoff are sparse in most regions. In contrast, river discharge is a hydrologic flux that is recorded regularly and with good accuracy for many of the world's major rivers. These measurements of discharge spatially integrate all upstream hydrological processes. As such, they can be used to evaluate distributed LSMs, but only if the simulated runoff is properly routed through the river basins. In this study, a rapid, computationally efficient source-to-sink (STS) routing scheme is presented that generates estimates of river discharge at gauge locations based on gridded runoff output. We applied the scheme as a postprocessor to archived output of the Global Land Data Assimilation System (GLDAS). GLDAS integrates satellite and ground-based data within multiple offline LSMs to produce fields of land surface states and fluxes. The application of the STS routing scheme allows for evaluation of GLDAS products in regions that lack distributed in situ hydrological measurements. We found that the four LSMs included in GLDAS yield very different estimates of river discharge and that there are distinct geographic patterns in the accuracy of each model as evaluated against gauged discharge. The choice of atmospheric forcing data set also had a significant influence on the accuracy of simulated discharge.
C1 [Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Olivera, Francisco] Texas A&M Univ, Zachry Dept Civil Engn, College Stn, TX 77843 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Zaitchik, BF (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 301 Olin Hall,3400 N Charles St, Baltimore, MD 21218 USA.
EM zaitchik@jhu.edu
RI Rodell, Matthew/E-4946-2012; Zaitchik, Benjamin/B-9461-2013
OI Rodell, Matthew/0000-0003-0106-7437;
FU NASA
FX The authors thank Hiroko Kato for performing the GLDAS simulations used
in this study and for providing insight on their results. The authors
also thank multiple members of the NASA Hydrological Sciences Branch for
contributing their ideas and technical expertise. The Global Runoff Data
Center (GRDC) is gratefully acknowledged for providing all river gauge
data used in this study. This work was funded by NASA's Energy and Water
Cycle Study (NEWS) program.
NR 79
TC 48
Z9 49
U1 1
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD JUN 10
PY 2010
VL 46
AR W06507
DI 10.1029/2009WR007811
PG 17
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 610OG
UT WOS:000278742000001
ER
PT J
AU Gong, J
Geller, MA
AF Gong, Jie
Geller, Marvin A.
TI Vertical fluctuation energy in United States high vertical resolution
radiosonde data as an indicator of convective gravity wave sources
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL LOWER STRATOSPHERE; MIDDLE ATMOSPHERE; MACQUARIE ISLAND;
INTERANNUAL VARIABILITY; LATITUDINAL VARIATIONS; GENERAL-CIRCULATION;
MOMENTUM FLUX; MODEL; PARAMETERIZATION; SPECTRUM
AB Convectively generated internal gravity waves at extratropical latitudes are difficult to identify by climatological analysis of the temperature and horizontal wind fields from radiosonde profiles using traditional analysis methods. Here, we show that, by analyzing ascent rate profiles (we define a new variable, "vertical fluctuation energy (VE)"), we can identify convection sources in climatological analyses. Analysis of a 9-year time series (1998-2006) of United States high vertical resolution radiosonde data shows that VE maximizes in summer in midlatitudes within the troposphere (2-8.9 km), and peaks at local afternoon-early evening during the summer over most of the contiguous United States. Furthermore, the apparent dominant vertical wavelength based on Fourier analysis of the low-pass filtered ascent rate fluctuations also increase and decrease with VE, both on diurnal and seasonal timescales. VE in the lower stratosphere, however, does not show this same relationship to convection, but analysis of the vertical wavelength does show some of the features seen in tropospheric VE. Unlike midlatitude stations, VE within both the troposphere and the lower stratosphere over tropical western Pacific island stations is highly correlated with convective precipitation and inversely correlated with outgoing longwave radiation. We interpret this difference by using the 4-D Gravity Wave Regional or Global Ray Tracer ray-tracing model with a source spectrum representative of a convection source.
C1 [Gong, Jie; Geller, Marvin A.] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA.
RP Gong, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jie.Gong@jpl.nasa.gov
RI Gong, Jie/H-2436-2011
FU NSF [ATM - 0413747]
FX This research is sponsored by NSF grant ATM - 0413747. The authors are
grateful to Joan Alexander, Brian Colle, Stephen Eckermann, and Kaoru
Sato for helpful discussions and suggestions. Three anonymous reviewers'
comments and suggestions are also greatly appreciated.
NR 54
TC 19
Z9 20
U1 2
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 9
PY 2010
VL 115
AR D11110
DI 10.1029/2009JD012265
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 610KZ
UT WOS:000278732900001
ER
PT J
AU Sultana, J
Kazanas, D
AF Sultana, Joseph
Kazanas, Demosthenes
TI Bending of light in conformal Weyl gravity
SO PHYSICAL REVIEW D
LA English
DT Article
ID COSMOLOGICAL CONSTANT; DEFLECTION; CLUSTERS; ENERGY; MATTER; LIMIT
AB We reexamine the bending of light issue associated with the metric of the static, spherically symmetric solution of Weyl gravity discovered by Mannheim and Kazanas (1989). To this end we employ the procedure used recently by Rindler and Ishak to obtain the bending angle of light by a centrally concentrated spherically symmetric matter distribution in a Schwarzschild-de Sitter background. In earlier studies the term gamma r in the metric led to the paradoxical result of a bending angle proportional to the photon impact parameter, when using the usual formalism appropriate to asymptotically flat space-times. However, employing the approach of light bending of Rindler and Ishak we show that the effects of this term are in fact insignificant, with the discrepancy between the two procedures attributed to the definition of the bending angle between the asymptotically flat and nonflat spaces.
C1 [Sultana, Joseph; Kazanas, Demosthenes] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Sultana, Joseph] Univ Malta, Dept Math, Msida, Malta.
RP Sultana, J (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
EM joseph.sultana@um.edu.mt; demos.kazanas@nasa.gov
FU NASA-GSFC
FX J. S. gratefully acknowledges the financial support of the Fulbright
Program, during his stay at NASA-GSFC.
NR 29
TC 21
Z9 21
U1 0
U2 3
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 JUN 9
PY 2010
VL 81
IS 12
AR 127502
DI 10.1103/PhysRevD.81.127502
PG 4
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 608BH
UT WOS:000278555900010
ER
PT J
AU Lu, GP
Blakeslee, RJ
Li, JB
Smith, DM
Shao, XM
McCaul, EW
Buechler, DE
Christian, HJ
Hall, JM
Cummer, SA
AF Lu, Gaopeng
Blakeslee, Richard J.
Li, Jingbo
Smith, David M.
Shao, Xuan -Min
McCaul, Eugene W.
Buechler, Dennis E.
Christian, Hugh J.
Hall, John M.
Cummer, Steven A.
TI Lightning mapping observation of a terrestrial gamma-ray flash
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID THUNDERSTORM; PROPAGATION; RADIATION; ARRAY
AB We report the observation with the North Alabama Lightning Mapping Array (LMA) related to a terrestrial gamma-ray flash (TGF) detected by RHESSI on 26 July 2008. The LMA data explicitly show the TGF was produced during the initial development of a compact intracloud (IC) lightning flash between a negative charge region centered at about 8.5 km above sea level (-22 degrees C temperature level) a higher positive region centered at 13 km, both confined to the convective core of an isolated storm in close proximity to the RHESSI footprint. After the occurrence of an LMA source with a high peak power (26 kW), the initial lightning evolution caused an unusually large IC current moment that became detectable 2 ms after the first LMA source and increased for another 2 ms, during which the burst of gamma-rays was produced. This slowly building current moment was most likely associated with the upward leader progression, which produced an uncommonly large IC charge moment change (+90 C.km) in 3 ms while being punctuated by a sequence of fast discharge. These observations suggest that the leader development may be involved in the TGF production. Citation: Lu, G., R. J. Blakeslee, J. Li, D. M. Smith, X. -M. Shao, E. W. McCaul, D. E. Buechler, H. J. Christian, J. M. Hall, and S. A. Cummer (2010), Lightning mapping observation of a terrestrial gamma-ray flash, Geophys. Res. Lett., 37, L11806, doi: 10.1029/2010GL043494.
C1 [Lu, Gaopeng; Li, Jingbo; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Blakeslee, Richard J.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
[Smith, David M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Shao, Xuan -Min] Los Alamos Natl Lab, Space & Remote Sensing Grp, Los Alamos, NM 87545 USA.
[McCaul, Eugene W.] Univ Space Res Assoc, Huntsville, AL 35806 USA.
[Buechler, Dennis E.; Christian, Hugh J.; Hall, John M.] Univ Alabama, Global Hydrol & Climate Ctr, Huntsville, AL 35806 USA.
RP Lu, GP (reprint author), Duke Univ, Dept Elect & Comp Engn, Box 90921, Durham, NC 27708 USA.
EM gl46@duke.edu; cummer@ee.duke.edu
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008
OI Cummer, Steven/0000-0002-0002-0613
FU NSF [ATM-0221968]
FX This work was supported by NSF Physical Meteorology Program grant
ATM-0221968. The authors would like to thank Bill Winn, Ken Eack, Ron
Thomas, Bill Rison, and David Raymond for valuable discussions.
NR 27
TC 59
Z9 59
U1 0
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 JUN 8
PY 2010
VL 37
AR L11806
DI 10.1029/2010GL043494
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 610KQ
UT WOS:000278732000005
ER
PT J
AU Xie, F
Wu, DL
Ao, CO
Kursinski, ER
Mannucci, AJ
Syndergaard, S
AF Xie, F.
Wu, D. L.
Ao, C. O.
Kursinski, E. R.
Mannucci, A. J.
Syndergaard, S.
TI Super-refraction effects on GPS radio occultation refractivity in marine
boundary layers
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LOWER TROPOSPHERE; SUPERREFRACTION; STRATOCUMULUS; ATMOSPHERE;
FEEDBACKS; SIGNALS
AB With the combination of global coverage, high vertical resolution, and all-weather capability, GPS radio occultation (RO) is an emerging satellite remote sensing technique that can probe the atmospheric boundary layer (ABL) on a global basis. However, a systematic negative bias (commonly referred to as N-bias) remains in derived refractivity profiles in the ABL. In this paper we present the N-biases in COSMIC RO soundings with respect to ECMWF analyses, which show a seasonally varying pattern clustered over the oceans where super-refraction (SR) often occurs. A case study of coincident COSMIC RO and radiosonde sounding confirms that the N-bias is primarily caused by SR. We also show that the high-rate RO bending angle measurements can resolve the ABL top at a vertical resolution better than 100 m. A reconstruction method is applied to one case where SR occurs and significantly reduces the negative refractivity error in the ABL. Citation: Xie, F., D. L. Wu, C. O. Ao, E. R. Kursinski, A. J. Mannucci, and S. Syndergaard (2010), Super-refraction effects on GPS radio occultation refractivity in marine boundary layers, Geophys. Res. Lett., 37, L11805, doi: 10.1029/2010GL043299.
C1 [Xie, F.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA.
[Xie, F.; Wu, D. L.; Ao, C. O.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kursinski, E. R.] Univ Arizona, Dept Atmospher Sci, Tucson, AZ 85721 USA.
[Syndergaard, S.] Danish Meteorol Inst, DK-2100 Copenhagen, Denmark.
RP Xie, F (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90024 USA.
EM feiqin.xie@jpl.nasa.gov
RI XIE, FEIQIN/J-4569-2013; Wu, Dong/D-5375-2012; Syndergaard,
Stig/C-1103-2017
OI Syndergaard, Stig/0000-0003-3119-2618
FU JIFRESSE at UCLA; NOAA JCSDA; National Aeronautics and Space
Administration (NASA)
FX This work was supported by an appointment to JIFRESSE at UCLA. Dr. F.
Xie and Dr. E. R. Kursinski are partly supported by NOAA JCSDA. Drs. D.
L. Wu, C. O. Ao and A. J. Mannucci are supported by the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration (NASA). ECMWF
analyses were provided by ECMWF through NCAR's CISL (Computational and
Information Systems Laboratory) Research Data Archive (RDA). The authors
would like to thank Byron Iijima, Marc Pestana, Tom Meehan, and Larry
Young at JPL for assistance with the COSMIC retrievals and helpful
discussions. We also thank Dr. Rick Anthe at UCAR and another anonymous
reviewer for their help to improve the manuscript.
NR 26
TC 14
Z9 14
U1 1
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 JUN 8
PY 2010
VL 37
AR L11805
DI 10.1029/2010GL043299
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 610KQ
UT WOS:000278732000004
ER
PT J
AU Klimas, A
Uritsky, V
Donovan, E
AF Klimas, Alex
Uritsky, Vadim
Donovan, Eric
TI Multiscale auroral emission statistics as evidence of turbulent
reconnection in Earth's midtail plasma sheet
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID SELF-ORGANIZED CRITICALITY; SPORADIC LOCALIZED RECONNECTIONS;
MAGNETIC-FIELD TOPOLOGY; FLOW BURSTS; INTERMITTENT TURBULENCE; COHERENT
STRUCTURES; SPACE PLASMAS; MT-INDEX; DYNAMIC MAGNETOSPHERE; PARTICLE
INJECTIONS
AB We provide indirect evidence for turbulent reconnection in Earth's midtail plasma sheet by reexamining the statistical properties of bright, nightside auroral emission events as observed by the UVI experiment on the Polar spacecraft and discussed previously by Uritsky et al. (2002, 2003, 2006). The events are divided into two groups: (1) those that map to vertical bar X-GSM vertical bar < 12 R-E in the magnetotail and do not show scale-free statistics and (2) those that map to vertical bar X-GSM vertical bar > 12 R-E and do show scale-free statistics. The vertical bar X-GSM vertical bar dependence is shown to most effectively organize the events into these two groups. Power law exponents obtained for group 2 are shown to validate the conclusions of Uritsky et al. concerning the existence of critical dynamics in the auroral emissions. It is suggested that the auroral dynamics is a reflection of a critical state in the magnetotail that is based on the dynamics of turbulent reconnection in the midtail plasma sheet.
C1 [Klimas, Alex] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Uritsky, Vadim; Donovan, Eric] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
RP Klimas, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM alex.klimas@nasa.gov
OI Donovan, Eric/0000-0002-8557-4155
FU NASA [NNX08AG73G]; MMS IDS [NCC5-494]
FX We would like to acknowledge the essential contributions to many aspects
of our results by D. Fairfield, A. Richmond, S. Boardsen, and N.
Tsyganenko. For this research, one of us (A.J.K.) was supported by NASA
grant NNX08AG73G and by the MMS IDS grant NCC5-494.
NR 76
TC 12
Z9 12
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN 8
PY 2010
VL 115
AR A06202
DI 10.1029/2009JA014995
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 610MV
UT WOS:000278738000004
ER
PT J
AU Corvino, G
Rezzolla, L
Bernuzzi, S
De Pietri, R
Giacomazzo, B
AF Corvino, Giovanni
Rezzolla, Luciano
Bernuzzi, Sebastiano
De Pietri, Roberto
Giacomazzo, Bruno
TI On the shear instability in relativistic neutron stars
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article; Proceedings Paper
CT Numerical Relativity Data Analysis Meeting
CY JUL 06-09, 2009
CL Albert Einstein Inst, Potsdam, GERMANY
HO Albert Einstein Inst
ID DIFFERENTIALLY ROTATING STARS; BAR-MODE INSTABILITY;
GRAVITATIONAL-RADIATION; DYNAMICAL INSTABILITIES; GENERAL-RELATIVITY;
ANGULAR-MOMENTUM; GROUND-STATE; DENSE MATTER; SIMULATIONS; STABILITY
AB We present new results on instabilities in rapidly and differentially rotating neutron stars. We model the stars in full general relativity and describe the stellar matter adopting a cold realistic equation of state based on the unified SLy prescription (Douchin and Haensel 2001 Astron. Astrophys. 380 151-67). We provide evidence that rapidly and differentially rotating stars that are below the expected threshold for the dynamical bar-mode instability, beta(c) T/vertical bar W vertical bar similar or equal to 0.25, do nevertheless develop a shear instability on a dynamical timescale and for a wide range of values of beta. This class of instability, which has so far been found only for small values of beta and with very small growth rates, is therefore more generic than previously found and potentially more effective in producing strong sources of gravitational waves. Overall, our findings support the phenomenological predictions made by Watts et al (2005 Astrophys. J. 618 L37) on the nature of the low-T/vertical bar W vertical bar instability as the manifestation of a shear instability in a region where the latter is possible only for small values of beta. Furthermore, our results provide additional insight on shear instabilities and on the necessary conditions for their development.
C1 [Corvino, Giovanni; Rezzolla, Luciano; Giacomazzo, Bruno] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Golm, Germany.
[Bernuzzi, Sebastiano] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany.
[De Pietri, Roberto] Univ Parma, Dept Phys, I-43100 Parma, Italy.
[De Pietri, Roberto] Ist Nazl Fis Nucl, Parma, Italy.
[Giacomazzo, Bruno] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacomazzo, Bruno] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
RP Corvino, G (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, Golm, Germany.
EM Giovanni.Corvino@roma1.infn.it
RI Corvino, Giovanni/D-5918-2011; Giacomazzo, Bruno/I-8088-2012; De Pietri,
Roberto/E-5336-2012
OI Giacomazzo, Bruno/0000-0002-6947-4023; De Pietri,
Roberto/0000-0003-1556-8304
NR 52
TC 25
Z9 25
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD JUN 7
PY 2010
VL 27
IS 11
AR 114104
DI 10.1088/0264-9381/27/11/114104
PG 20
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 593KR
UT WOS:000277454000015
ER
PT J
AU Kelly, BJ
Tichy, W
Zlochower, Y
Campanelli, M
Whiting, B
AF Kelly, B. J.
Tichy, W.
Zlochower, Y.
Campanelli, M.
Whiting, B.
TI Post-Newtonian initial data with waves: progress in evolution
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article; Proceedings Paper
CT Numerical Relativity Data Analysis Meeting
CY JUL 06-09, 2009
CL Albert Einstein Inst, Potsdam, GERMANY
HO Albert Einstein Inst
ID 3-DIMENSIONAL CARTESIAN GRIDS; APPARENT-HORIZON FINDER; MANY-BODY
SYSTEM; NUMERICAL RELATIVITY; CANONICAL FORMALISM; BLACK-HOLES; ADM
AB In Kelly et al (2007 Phys. Rev. D 76 024008), we presented new binary black-hole initial data adapted to puncture evolutions in numerical relativity. These data satisfy the constraint equations to 2.5 post-Newtonian order, and contain a transverse-traceless 'wavy' metric contribution, violating the standard assumption of conformal flatness. We report on progress in evolving these data with a modern moving puncture implementation of the BSSN equations in several numerical codes. We discuss the effect of the new metric terms on junk radiation and continuity of physical radiation extracted.
C1 [Kelly, B. J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Kelly, B. J.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Kelly, B. J.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Tichy, W.] Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA.
[Zlochower, Y.; Campanelli, M.] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Sch Math Sci, Rochester, NY 14623 USA.
[Whiting, B.] Univ Florida, Dept Phys, Inst Fundamental Theory, Gainesville, FL 32611 USA.
RP Kelly, BJ (reprint author), NASA, Goddard Space Flight Ctr, CRESST, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM bernard.j.kelly@nasa.gov
RI Kelly, Bernard/G-7371-2011;
OI Kelly, Bernard/0000-0002-3326-4454; Whiting, Bernard
F/0000-0002-8501-8669
NR 34
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD JUN 7
PY 2010
VL 27
IS 11
AR 114005
DI 10.1088/0264-9381/27/11/114005
PG 11
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 593KR
UT WOS:000277454000007
ER
PT J
AU Rezzolla, L
Baiotti, L
Giacomazzo, B
Link, D
Font, JA
AF Rezzolla, Luciano
Baiotti, Luca
Giacomazzo, Bruno
Link, David
Font, Jose A.
TI Accurate evolutions of unequal-mass neutron-star binaries: properties of
the torus and short GRB engines
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article; Proceedings Paper
CT Numerical Relativity Data Analysis Meeting
CY JUL 06-09, 2009
CL Albert Einstein Inst, Potsdam, GERMANY
HO Albert Einstein Inst
ID GAMMA-RAY BURSTS; QUASI-PERIODIC OSCILLATIONS; SCHWARZSCHILD BLACK-HOLE;
RUNAWAY INSTABILITY; RELATIVISTIC TORI; ANGULAR-MOMENTUM; THICK DISCS;
NUMERICAL RELATIVITY; GRAVITATIONAL-WAVES; ACCRETION DISKS
AB We present new results from accurate and fully general-relativistic simulations of the coalescence of unmagnetized binary neutron stars with various mass ratios. The evolution of the stars is followed through the inspiral phase, the merger, and the prompt collapse to a black hole, up until the appearance of a thick accretion disc, which is studied as it enters and remains in a regime of quasi-steady accretion. Although a simple ideal-fluid equation of state with Gamma = 2 is used, this work presents a systematic study within a fully general-relativistic framework of the properties of the resulting black-hole-torus system produced by the merger of unequal-mass binaries. More specifically, we show that (1) the mass of the torus increases considerably with the mass asymmetry, and equal-mass binaries do not produce significant tori if they have a total baryonic mass M(tot) greater than or similar to 3.7 M(circle dot); (2) tori with masses M(tor) similar to 0.2 M(circle dot) are measured for binaries with M(tot) similar to 3.4 M(circle dot) and mass ratios q similar to 0.75-0.85; (3) the mass of the torus can be estimated by the simple expression (M) over tilde (tor) (q, M(tot)) = [c(1)(1 - q) + c(2)] (M(max) - M(tot)), involving the maximum mass for the binaries and coefficients constrained from the simulations, and suggesting that the tori can have masses as large as (M) over tilde (tor) similar to 0.35 M(circle dot) for M(tot) similar to 2.8 M(circle dot) and q similar to 0.75-0.85; (4) using a novel technique to analyze the evolution of the tori, we find no evidence for the onset of non-axisymmetric instabilities and that very little, if any, of their mass is unbound; (5) finally, for all the binaries considered, we compute the complete gravitational waveforms and the recoils imparted to the black holes, discussing the prospects of the detection of these sources for a number of present and future detectors.
C1 [Rezzolla, Luciano; Giacomazzo, Bruno; Link, David] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Potsdam, Germany.
[Baiotti, Luca] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 606, Japan.
[Giacomazzo, Bruno] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacomazzo, Bruno] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Link, David] Humboldt Univ, Inst Phys, Berlin, Germany.
[Font, Jose A.] Univ Valencia, Dept Astron & Astrofis, Valencia, Spain.
RP Rezzolla, L (reprint author), Max Planck Inst Gravitat Phys, Albert Einstein Inst, Potsdam, Germany.
EM rezzolla@aei.mpg.de
RI Giacomazzo, Bruno/I-8088-2012
OI Giacomazzo, Bruno/0000-0002-6947-4023
NR 76
TC 95
Z9 96
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD JUN 7
PY 2010
VL 27
IS 11
AR 114105
DI 10.1088/0264-9381/27/11/114105
PG 36
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 593KR
UT WOS:000277454000016
ER
PT J
AU Fonti, S
Montanaro, S
Politi, R
Blanco, A
Marra, AC
Marzo, GA
Orofino, V
AF Fonti, S.
Montanaro, S.
Politi, R.
Blanco, A.
Marra, A. C.
Marzo, G. A.
Orofino, V.
TI Infrared reflectance spectra of particulate mixtures
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID EMISSION-SPECTROSCOPY; COHERENT BACKSCATTER; MINERAL MIXTURES;
PARTICLES; SCATTERING; REGOLITHS; QUARTZ
AB In this work we report the main results of a laboratory test program aimed to check the spectral behavior of several mixtures of particulate samples. The chosen spectral interval is from 2.5 to 25.0 mu m since it is the range where many minerals have their characteristic features and it is important for the interpretation of remote sensing spectra of planetary surfaces. The present study uses directional hemispherical reflectance spectra of three particulate minerals (dolomite, olivine, and quartz), with different grain sizes (ranging from 1 to 300 mu m), and of their mixtures. It was found that, in the spectral range between 2.5 mu m and the Christiansen feature, the reflectance of the mixtures is a nonlinear combination of the reflectance of the single pure materials, in agreement with the results found at shorter wavelength and reported in the literature. Our experimental results also confirm that, for longer wavelength, the reflectance of the mixtures is a linear combination of the reflectance of the single pure minerals. In this work, after checking some important simplifying hypotheses, we show that the mixture spectra cannot be always accurately reproduced using the volume percentage of each component, but it has a complicate behavior requiring a careful evaluation of all the parameters involved in the process. In particular we have determined experimentally the penetration depth of the radiation at different wavelengths in some of the mixtures. In this way we have been able to address the important issue of the influence of surface composition on the observed spectra.
C1 [Fonti, S.; Montanaro, S.; Blanco, A.; Orofino, V.] Univ Salento, Dept Phys, I-73100 Lecce, Italy.
[Politi, R.] INAF, IASF, I-00133 Rome, Italy.
[Marra, A. C.] CNR, ISAC, I-73100 Lecce, Italy.
[Marzo, G. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Fonti, S (reprint author), Univ Salento, Dept Phys, Via Arnesano,CP 193, I-73100 Lecce, Italy.
EM sergio.fonti@le.infn.it
RI Marzo, Giuseppe/A-9765-2015;
OI Politi, Romolo/0000-0002-9793-9780
FU Ministry of University and Research; Italian Space Agency; National
Institute of Astrophysics
FX This research has been partially supported by the Ministry of University
and Research, the Italian Space Agency, and the National Institute of
Astrophysics. The authors warmly thank Ljuba Moroz for her constructive
discussion and valuable suggestions, as well as Bruce Hapke and Bethany
Ehlmann for their very useful reviews that allowed us to considerably
improve the quality of the manuscript.
NR 28
TC 1
Z9 1
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JUN 5
PY 2010
VL 115
AR E06003
DI 10.1029/2009JE003461
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 606UW
UT WOS:000278454800002
ER
PT J
AU Zhao, MH
Gu, XH
Lowther, SE
Park, C
Jean, YC
Nguyen, T
AF Zhao, Minhua
Gu, Xiaohong
Lowther, Sharon E.
Park, Cheol
Jean, Y. C.
Nguyen, Tinh
TI Subsurface characterization of carbon nanotubes in polymer composites
via quantitative electric force microscopy
SO NANOTECHNOLOGY
LA English
DT Article
ID SCANNING PROBE MICROSCOPY; CONDUCTANCE MICROSCOPY; FIELD-EMISSION;
NETWORKS
AB Subsurface characterization of carbon nanotubes (CNTs) dispersed in free-standing polymer composite films was achieved via quantitative electric force microscopy (EFM). The effects of relative humidity, EFM probe geometry, tip-sample distance and bias voltage on the EFM contrast were studied. Non-parabolic voltage dependence of the EFM signal of subsurface CNTs in polymer composites was observed and a new mechanism was proposed taking consideration of capacitive coupling as well as coulombic coupling. We anticipate that this quantitative EFM technique will be a useful tool for non-destructive subsurface characterization of high dielectric constant nanostructures in low dielectric constant matrices.
C1 [Zhao, Minhua; Gu, Xiaohong; Nguyen, Tinh] NIST, Mat & Construct Res Div, Gaithersburg, MD 20899 USA.
[Lowther, Sharon E.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Park, Cheol] Natl Inst Aerosp, Hampton, VA 23681 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Jean, Y. C.] Univ Missouri, Dept Chem, Kansas City, MO 64110 USA.
RP Zhao, MH (reprint author), NIST, Mat & Construct Res Div, Gaithersburg, MD 20899 USA.
EM minhua.zhao@nist.gov; tinh.nguyen@nist.gov
RI Zhao, Minhua/A-6678-2009
OI Zhao, Minhua/0000-0003-4880-1010
FU NIST/NIH(NIBIB)
FX The first author (MZ) acknowledges the support of a National Research
Council Fellowship sponsored by NIST/NIH(NIBIB).
NR 46
TC 34
Z9 34
U1 0
U2 24
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD JUN 4
PY 2010
VL 21
IS 22
AR 225702
DI 10.1088/0957-4484/21/22/225702
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 592UL
UT WOS:000277405900012
PM 20453284
ER
PT J
AU Naud, CM
Del Genio, AD
Haeffelin, M
Morille, Y
Noel, V
Dupont, JC
Turner, DD
Lo, C
Comstock, J
AF Naud, C. M.
Del Genio, A. D.
Haeffelin, M.
Morille, Y.
Noel, V.
Dupont, J. -C.
Turner, D. D.
Lo, C.
Comstock, J.
TI Thermodynamic phase profiles of optically thin midlatitude clouds and
their relation to temperature
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ACTIVE REMOTE SENSORS; ICE WATER-CONTENT; LIDAR DEPOLARIZATION; AIRCRAFT
OBSERVATIONS; PRECIPITATION SCHEME; MULTIPLE-SCATTERING; RAMAN LIDAR;
RADAR; CLIMATE; VAPOR
AB The relationship between cloud thermodynamic phase and temperature in some aircraft measurements conducted in midlatitude frontal clouds suggests that significant liquid does not exist at temperatures colder than 258 K. This data set is often used to verify parameterizations of cloud phase in general circulation models. However, other aircraft campaigns and different instruments suggest a different relationship. Here we examine the temperature-phase relationship for midlatitude optically thin winter clouds. Cloud phase and temperature profiles derived from 5 years of ground-based lidar depolarization and radiosonde measurements are analyzed for two midlatitude locations: the U. S. Atmospheric Radiation Measurement Program Southern Great Plains site and the Site Instrumental de Recherche par Teledetection Atmospherique in France. Because lidars are attenuated in optically thick clouds, the data set only includes clouds with optical thickness of < 3. Cloud phase is obtained by using the classical method based on a depolarization ratio threshold of 11% for differentiating liquid from ice. The frequency of occurrence of clouds either completely liquid or completely glaciated in the temperature range from 233 to 273 K is similar to previous observations in the midlatitudes but somewhat greater than in the Arctic. The relationship between ice phase occurrence and temperature only slightly changes between cloud base and top. At both sites, liquid is more prevalent at colder temperatures than has been found previously in some thicker frontal clouds, suggesting different processes for glaciation in nonfrontal optically thin clouds.
C1 [Naud, C. M.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
[Naud, C. M.; Del Genio, A. D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Haeffelin, M.; Morille, Y.; Noel, V.; Dupont, J. -C.] Ecole Polytech, Meteorol Dynam Lab, F-91128 Palaiseau, France.
[Haeffelin, M.; Morille, Y.; Noel, V.; Dupont, J. -C.] Ecole Polytech, Inst Pierre Simon Laplace, F-91128 Palaiseau, France.
[Turner, D. D.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Lo, C.; Comstock, J.] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Naud, CM (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10027 USA.
EM cnaud@giss.nasa.gov
RI Del Genio, Anthony/D-4663-2012; Noel, Vincent/C-3702-2013
OI Del Genio, Anthony/0000-0001-7450-1359; Noel,
Vincent/0000-0001-9494-0340
FU U. S. Department of Energy [DE-FG02-06ER64167]
FX This work was supported by an Interagency Agreement with the Atmospheric
Radiation Measurement program of the U. S. Department of Energy. Support
for D. Turner was provided by grant DE-FG02-06ER64167 from DOE BER as
part of the ARM program.
NR 58
TC 11
Z9 11
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 3
PY 2010
VL 115
AR D11202
DI 10.1029/2009JD012889
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 606UI
UT WOS:000278453400004
ER
PT J
AU Hillan, DS
Cairns, IH
Robinson, PA
Mohamed, A
AF Hillan, D. S.
Cairns, Iver H.
Robinson, P. A.
Mohamed, A.
TI Prediction of background levels for the Wind WAVES instrument and
implications for the galactic background radiation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID THERMAL NOISE; RADIO-EMISSION; PLASMA; FREQUENCY; SPACECRAFT; ANTENNAS;
SHOCKS
AB We investigate and predict the observed background levels for the TNR, RAD1, and RAD2 receivers when connected to the X, Y, and Z antennas of the WAVES instrument on the spacecraft Wind. The receivers are connected to either a single antenna, in "SEP" mode, or a combination of antennas, in "SUM" mode. With the TNR receiver in SEP (X) mode, the predicted backgrounds agree to within 20% when modeled using a two component model for the quasi-thermal plasma noise (QTN). Calibrating the RAD1 in SEP (X) mode observations against TNR allows us to calculate the relative receiver gain G(R1) = 1.43 +/- 0.18. Using the RAD1 data in SUM (X + Z) mode, the ratio of antenna gains is found to be R = 6.5, in agreement with preflight measurements. Observed differences between the SEP (X) and SUM (X + Z) modes are explained for the first time, and the predicted levels of QTN and galactic background are found to agree to within 20%. RAD2 is also calibrated against RAD1 and TNR, yielding a total gain G(R2)G(y) = 2.5 +/- 0.3. Differences between the predicted and observed galactic background spectra are used to estimate the effective antenna lengths for the X and Y antennas, which are found to be between the physical monopole antenna length L and the Hansen (1981) prediction of root(2/3)L. The analyses are consistent with the Novaco and Brown (1978) galactic background model, which decreases much faster than that of Cane (1979). Our model background spectrum is useful for theory-data comparisons of type II and III bursts.
C1 [Hillan, D. S.; Cairns, Iver H.; Robinson, P. A.; Mohamed, A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Mohamed, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hillan, DS (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
EM hillan@physics.usyd.edu.au
OI Cairns, Iver/0000-0001-6978-9765
FU Australian Research Council
FX We thank S. Hoang, P. J. Kellogg, M. L. Kaiser, M. Maksimovic, K.
Issautier, and J. Eastwood for helpful discussions. The Australian
Research Council supported this research.
NR 21
TC 3
Z9 3
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JUN 2
PY 2010
VL 115
AR A06102
DI 10.1029/2009JA014714
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 606VB
UT WOS:000278455300001
ER
PT J
AU Shakya, KM
Ziemba, LD
Griffin, RJ
AF Shakya, Kabindra M.
Ziemba, Luke D.
Griffin, Robert J.
TI Characteristics and Sources of Carbonaceous, Ionic, and Isotopic Species
of Wintertime Atmospheric Aerosols in Kathmandu Valley, Nepal
SO AEROSOL AND AIR QUALITY RESEARCH
LA English
DT Article
DE Carbonaceous aerosols; Kathmandu; Ionic aerosols; Isotope ratios
ID ELEMENTAL CARBON; SOURCE APPORTIONMENT; ORGANIC AEROSOL;
CHEMICAL-COMPOSITION; AIR-POLLUTION; CHINA; PARTICLES; PM2.5;
PARTICULATE; COMPONENTS
AB To investigate the air pollution from aerosols in Kathmandu during winter, bulk aerosol samples were collected during winter 2007-2008 to characterize carbonaceous and ionic species and carbon and nitrogen isotopes. This study illustrates the applications of carbon and nitrogen isotope data for characterizing aerosols and their implications for identifying sources that were inconsistent with the results for the carbonaceous and ionic aerosols. Mean concentrations of organic carbon (OC), elemental carbon (EC), and water soluble organic carbon (WSOC) in Kathmandu during the period were 20.02 +/- 6.59 (1 sigma), 4.48 +/- 1.17, and 10.09 +/- 3.64 mu gC/m(3), respectively. Elemental carbon and OC were correlated (R(2) = 0.56), likely indicating common sources for both species, as well as for the precursors that led to the formation of secondary organic carbon (SOC). The mean estimated SOC contribution to OC was 31%, suggesting that local emission is more important than transport and processing during winter in Kathmandu. On average, 50% of the OC was water soluble, and the correlation of SOC with WSOC (R(2) = 0.66) suggests that the majority of SOC and some primary organic carbon (POC) were water soluble in Kathmandu. The mean delta(13)C of -25.74 +/- 0.19 parts per thousand observed in aerosols of Kathmandu confirms consistent anthropogenic sources such as fossil fuel combustion. Heavier carbon also was observed to be associated with the water-soluble fraction of OC in aerosols. The mean delta(15)N of 9.45 +/- 0.87 parts per thousand suggests the limited influence of biomass burning and its strong correlation with crustal cations Ca(2+) (R(2) = 0.74, p < 0.05) and Mg(2+) (R(2) = 0.71, p < 0.05) indicates distant sources. Principal component analysis revealed four major sources/pathways for particles: local and vehicular emissions, secondary gas-to-particle conversion, aqueous processing, and dust transport, each explaining similar to 39, 23, 11, and 9% of the variance.
C1 [Shakya, Kabindra M.; Griffin, Robert J.] Rice Univ, Dept Civil & Environm Engn, Houston, TX 77005 USA.
[Shakya, Kabindra M.; Ziemba, Luke D.; Griffin, Robert J.] Univ New Hampshire, Climate Change Res Ctr, Durham, NH 03824 USA.
[Ziemba, Luke D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Griffin, RJ (reprint author), Rice Univ, Dept Civil & Environm Engn, 6100 Main St, Houston, TX 77005 USA.
EM rob.griffin@rice.edu
RI Wang, Linden/M-6617-2014
FU University of New Hampshire
FX The partial support of the University of New Hampshire Ph.D. program in
Natural Resources and Earth System Sciences, Andrew Quimette and Philip
Place for help in isotope analyses, and Neeraj Tamrakar for providing
the sampling site and logistical support are gratefully acknowledged.
NR 46
TC 22
Z9 22
U1 1
U2 25
PU TAIWAN ASSOC AEROSOL RES-TAAR
PI TAICHUNG COUNTY
PA CHAOYANG UNIV TECH, DEPT ENV ENG & MGMT, PROD CTR AAQR, NO 168, JIFONG E
RD, WUFONG TOWNSHIP, TAICHUNG COUNTY, 41349, TAIWAN
SN 1680-8584
J9 AEROSOL AIR QUAL RES
JI Aerosol Air Qual. Res.
PD JUN
PY 2010
VL 10
IS 3
BP 219
EP U13
DI 10.4209/aaqr.2009.10.0068
PG 13
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 580NK
UT WOS:000276455900003
ER
PT J
AU Sietzen, F
Aldrin, B
AF Sietzen, Frank
Aldrin, Buzz
TI Conversations with Buzz Aldrin
SO AEROSPACE AMERICA
LA English
DT Editorial Material
C1 [Aldrin, Buzz] NASA, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD JUN
PY 2010
VL 48
IS 6
BP 12
EP 14
PG 3
WC Engineering, Aerospace
SC Engineering
GA V24JR
UT WOS:000208407200004
ER
PT J
AU Kirk, BS
Carey, GF
AF Kirk, Benjamin S.
Carey, Graham F.
TI Validation of Fully Implicit, Parallel Finite Element Simulations of
Laminar Hypersonic Flows
SO AIAA JOURNAL
LA English
DT Article
ID COMPUTATIONAL FLUID-DYNAMICS; NAVIER-STOKES EQUATIONS;
ADVECTIVE-DIFFUSIVE SYSTEMS; COMPRESSIBLE EULER; FORMULATION; ALGORITHM;
OPERATOR; SCIENCE; SCHEME
AB This paper concerns comparative studies of predictive simulations and experimental results from the literature for high-Mach-number two-dimensional/axisymmetric flow past a hollow-cylinder flare and a double cone. The underlying physical model for the mathematical formulation assumes calorically-perfect-gas laminar flow, and we seek to approximate the corresponding compressible Navier-Stokes equations expressed in conservation-variable form. Predictive simulations of this mathematical model are based on a fully implicit, parallel streamline-upwind Petrov-Galerkin finite element formulation that uses a grouped-variable expansion for the inviscid flux terms. The spatial discretization, second-order-accurate time discretization, numerical method, and parallel fully implicit implementation are concisely described. Representative iterative and mesh convergence results are presented for the case of a hollow-cylinder flare. Local predicted values of surface pressure and heat transfer are compared with available experimentally measured values for both geometries. These results are interpreted in the context of validation. Predicted results for complex flowfield/shock interactions and the viscous slip surface are illustrated through a computed schlieren image for the double cone. The present work presents the first known comparison of predictions from the finite element method to this set of data, and the validation study provides the comparative details to motivate future computational investigations and experimental studies.
C1 [Kirk, Benjamin S.] NASA, Lyndon B Johnson Space Ctr, Appl Aerosci & Computat Fluid Dynam Branch, Houston, TX 77058 USA.
[Carey, Graham F.] Univ Texas Austin, Inst Computat Engn Sci, Austin, TX 78712 USA.
RP Kirk, BS (reprint author), NASA, Lyndon B Johnson Space Ctr, Appl Aerosci & Computat Fluid Dynam Branch, 2101 NASA Pkwy,Mail Code EG3, Houston, TX 77058 USA.
NR 48
TC 0
Z9 1
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD JUN
PY 2010
VL 48
IS 6
BP 1025
EP 1036
DI 10.2514/1.40860
PG 12
WC Engineering, Aerospace
SC Engineering
GA 605MY
UT WOS:000278352900001
ER
PT J
AU Nielsen, EJ
Diskin, B
Yamaleev, NK
AF Nielsen, Eric J.
Diskin, Boris
Yamaleev, Nail K.
TI Discrete Adjoint-Based Design Optimization of Unsteady Turbulent Flows
on Dynamic Unstructured Grids
SO AIAA JOURNAL
LA English
DT Article
ID NAVIER-STOKES EQUATIONS; SENSITIVITY-ANALYSIS; COMPLEX-VARIABLES;
MESHES; ALGORITHM; IMPLICIT; SYSTEMS
AB An adjoint-based methodology for design optimization of unsteady turbulent flows on dynamic unstructured grids is described. The implementation relies on an existing unsteady three-dimensional unstructured grid solver capable of dynamic mesh simulations and discrete adjoint capabilities previously developed for steady flows. The discrete equations for the primal and adjoint systems are presented for the backward-difference family of time-integration schemes on both static and dynamic grids. The consistency of sensitivity derivatives is established via comparisons with complex-variable computations. The current work is believed to be the first verified implementation of an adjoint-based optimization methodology for the true time-dependent formulation of the Navier-Stokes equations in a practical computational code. Large-scale shape optimizations are demonstrated for turbulent flows over a tiltrotor geometry and a simulated aeroelastic motion of a fighter jet.
C1 [Nielsen, Eric J.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Yamaleev, Nail K.] N Carolina Agr & Tech State Univ, Dept Math, Greensboro, NC 27411 USA.
RP Nielsen, EJ (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
FU NASA [NNL07AA23C]
FX The authors wish to thank Robert Biedron of NASA Langley Research Center
for many useful discussions pertaining to the current work. Geometric
parameterizations provided by Bill Jones of NASA Langley Research Center
are also appreciated. Jan-Renee Carlson of NASA Langley Research Center
is acknowledged for her assistance with plenum geometry modifications
and boundary conditions for the fighter jet example. The second and
third authors acknowledge the support from NASA under grant NNL07AA23C.
NR 43
TC 22
Z9 25
U1 1
U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD JUN
PY 2010
VL 48
IS 6
BP 1195
EP 1206
DI 10.2514/1.J050035
PG 12
WC Engineering, Aerospace
SC Engineering
GA 605MY
UT WOS:000278352900016
ER
PT J
AU Ho, JC
Hodges, DH
Yu, WB
AF Ho, Jimmy C.
Hodges, Dewey H.
Yu, Wenbin
TI Energy Transformation to Generalized Timoshenko Form for Nonuniform
Beams
SO AIAA JOURNAL
LA English
DT Article
ID SECTION
C1 [Hodges, Dewey H.] Georgia Inst Technol, Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Yu, Wenbin] Utah State Univ, Dept Mech & Aerosp Engn, Logan, UT 84322 USA.
RP Ho, JC (reprint author), USA, ELORET Corp, Aeroflightdynam Directorate, Ames Res Ctr, Mail Stop 215-1, Moffett Field, CA 94035 USA.
EM jimmy.c.ho@us.army.mil; dhodges@gatech.edu; wenbin@engineering.usu.edu
RI Yu, Wenbin/B-1916-2009
FU U.S. Army Vertical Lift Research Center of Excellence at Georgia
Institute of Technology
FX This research is supported by the U.S. Army Vertical Lift Research
Center of Excellence at Georgia Institute of Technology and its
affiliate program through subcontract at Utah State University. The
Technical Monitor is Michael J. Rutkowski.
NR 13
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 0001-1452
J9 AIAA J
JI AIAA J.
PD JUN
PY 2010
VL 48
IS 6
BP 1268
EP 1272
DI 10.2514/1.J050160
PG 5
WC Engineering, Aerospace
SC Engineering
GA 605MY
UT WOS:000278352900025
ER
PT J
AU Barker, CM
Johnson, WO
Eldridge, BF
Park, BK
Melton, F
Reisen, WK
AF Barker, Christopher M.
Johnson, Wesley O.
Eldridge, Bruce F.
Park, Bborie K.
Melton, Forrest
Reisen, William K.
TI Temporal Connections between Culex tarsalis Abundance and Transmission
of Western Equine Encephalomyelitis Virus in California
SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE
LA English
DT Article
ID ST-LOUIS ENCEPHALITIS; VECTOR COMPETENCE; TEMPERATURE; CULICIDAE;
DIPTERA; MOSQUITOS; VALLEY; ARBOVIRUSES; COACHELLA; INFECTION
AB Definition of targets for vector control requires an understanding of the relationship between vector abundance and the intensity of arbovirus transmission. Using an extensive surveillance dataset with observations from sentinel chicken flocks and mosquito traps paired in time and space, hierarchical autoregressive logistic regression models were developed to predict the probability of seroconversion in chickens for western equine encephalomyelitis virus (WEEV) based on the relative abundance of the principal vector, Culex tarsalis. After adjustments for confounders, the abundance of Cx. tarsalis 29-42 d before the date of chicken sampling was credibly associated with the risk of WEEV transmission in both the Central and Coachella Valleys, and a doubling of relative Cx. tarsalis abundance was associated with a 58% increase in the odds of seroconversion. The critical time windows identified in our study highlight the need for surveillance of vector populations and forecasting models to guide proactive vector control measures before the detection of transmission to sentinel chickens.
C1 [Barker, Christopher M.; Eldridge, Bruce F.; Park, Bborie K.; Reisen, William K.] Univ Calif Davis, Ctr Vectorborne Dis, Davis, CA 95616 USA.
[Johnson, Wesley O.] Univ Calif Irvine, Dept Stat, Donald Bren Sch Informat & Comp Sci, Irvine, CA USA.
Calif State Univ, Seaside, CA USA.
[Melton, Forrest] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NIH, Fogarty Int Ctr, Bethesda, MD 20892 USA.
RP Barker, CM (reprint author), Univ Calif Davis, Ctr Vectorborne Dis, Old Davis Rd, Davis, CA 95616 USA.
EM cmbarker@ucdavis.edu
FU NASA [RM08-6044, NNA06CN02A]; NOAA Office of Global Programs, Climate
Variability and Human Health [00-543]
FX This work was funded by NASA Earth-Sun Science Applied Sciences Program
Research Opportunities in Space and Earth Science, Decision Support
through Earth-Sun Science Research Results grant RM08-6044 for
NNA06CN02A and NOAA Office of Global Programs, Climate Variability and
Human Health grant 00-543.
NR 53
TC 2
Z9 2
U1 0
U2 4
PU AMER SOC TROP MED & HYGIENE
PI MCLEAN
PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA
SN 0002-9637
J9 AM J TROP MED HYG
JI Am. J. Trop. Med. Hyg.
PD JUN
PY 2010
VL 82
IS 6
BP 1185
EP 1193
DI 10.4269/ajtmh.2010.09-0324
PG 9
WC Public, Environmental & Occupational Health; Tropical Medicine
SC Public, Environmental & Occupational Health; Tropical Medicine
GA 606XP
UT WOS:000278462600036
PM 20519621
ER
PT J
AU Mckay, CP
AF McKay, Christopher P.
TI Liquid water formation around rocks and meteorites on Antarctic Polar
Plateau ice
SO ANTARCTIC SCIENCE
LA English
DT Article
ID CRYPTOENDOLITHIC MICROBIAL ENVIRONMENT; ALLAN HILLS 84001; AMINO-ACIDS;
ALH84001; CHONDRITES; DESERT; SEARCH
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Mckay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
NR 14
TC 3
Z9 3
U1 0
U2 13
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0954-1020
J9 ANTARCT SCI
JI Antarct. Sci.
PD JUN
PY 2010
VL 22
IS 3
BP 287
EP 288
DI 10.1017/S0954102010000118
PG 2
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 627CH
UT WOS:000280015800011
ER
PT J
AU Arkoosh, MR
Boylen, D
Dietrich, J
Anulacion, BF
Ylitalo, G
Bravo, CF
Johnson, LL
Loge, FJ
Collier, TK
AF Arkoosh, Mary R.
Boylen, Deborah
Dietrich, Joseph
Anulacion, Bernadita F.
Ylitalo, Gina
Bravo, Claudia F.
Johnson, Lyndal L.
Loge, Frank J.
Collier, Tracy K.
TI Disease susceptibility of salmon exposed to polybrominated diphenyl
ethers (PBDEs)
SO AQUATIC TOXICOLOGY
LA English
DT Article
DE PBDEs; Salmon; Disease susceptibility; Willamette River; Immune system;
Columbia River Basin; Listonella anguillarum
ID JUVENILE CHINOOK SALMON; POLYCHLORINATED-BIPHENYLS PCBS; BROMINATED
FLAME RETARDANTS; THYROID-HORMONES; COLUMBIA RIVER; IMMUNE-SYSTEM;
VITAMIN-A; ESTUARY; FISH; ENVIRONMENT
AB The health effects of the flame retardant polybrominated diphenyl ethers (PBDEs) in fish are not well understood. To determine the potential effects of this ubiquitous contaminant class on fish health, juvenile subyearling Chinook salmon (Oncorhynchus tshawytscha) were fed a diet that reflected the PBDE congeners found in the stomach contents of subyearling Chinook salmon collected from the highly urbanized and industrialized lower Willamette River in the Columbia River Basin of North America. The diet, consisting of five PBDE congeners (BDE-47, BDE-99, BDE-100, BDE-153 and BDE-154), was fed to the salmon at 2% of their body weight in food per day for 40 days. Two concentrations of the diet (1 x and 10x PBDE) were fed to the salmon. The 1x PBDE diet reflected the concentration of PBDEs (190 ng PBDEs/g food) found in the stomach contents of juvenile subyearling Chinook salmon; the 10x diet was prepared at 10 times that concentration. The fish were then exposed to the marine bacterial pathogen Listonella anguillarum to assess susceptibility to infectious disease. juvenile Chinook salmon fed the 1x PBDE diet were more susceptible to L. anguillarum than salmon fed the control diet. This suggests that juvenile salmonids in the lower Willamette River exposed to PBDEs may be at greater risk for disease than nonexposed juvenile salmonids. In contrast, salmon that consumed the 10x PBDE diet were not more susceptible to the pathogen than salmon fed the control diet. The mechanisms for the dichotomous results observed in disease susceptibility between salmon fed the 1x and 10x PBDE diets are currently not known but have also been observed in other species exposed to PBDEs with respect to immune function. Published by Elsevier B.V.
C1 [Arkoosh, Mary R.; Boylen, Deborah; Dietrich, Joseph] Natl Marine Fisheries Serv, Environm Conservat Div, NW Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Newport, OR 97365 USA.
[Anulacion, Bernadita F.; Ylitalo, Gina; Johnson, Lyndal L.; Collier, Tracy K.] Natl Marine Fisheries Serv, Environm Conservat Div, NW Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Seattle, WA 98112 USA.
[Bravo, Claudia F.; Loge, Frank J.] Univ Calif Davis, Dept Civil & Environm Engn, Davis, CA 95616 USA.
RP Arkoosh, MR (reprint author), Natl Marine Fisheries Serv, Environm Conservat Div, NW Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, 2032 SE OSU Dr, Newport, OR 97365 USA.
EM mary.arkoosh@noaa.gov
NR 49
TC 24
Z9 28
U1 5
U2 36
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0166-445X
J9 AQUAT TOXICOL
JI Aquat. Toxicol.
PD JUN 1
PY 2010
VL 98
IS 1
BP 51
EP 59
DI 10.1016/j.aquatox.2010.01.013
PG 9
WC Marine & Freshwater Biology; Toxicology
SC Marine & Freshwater Biology; Toxicology
GA 607LZ
UT WOS:000278506900007
PM 20207027
ER
PT J
AU Hintze, PE
Nicholson, WL
AF Hintze, Paul E.
Nicholson, Wayne L.
TI Single-spore elemental analyses indicate that dipicolinic acid-deficient
Bacillus subtilis spores fail to accumulate calcium
SO ARCHIVES OF MICROBIOLOGY
LA English
DT Article
DE Bacillus subtilis; Spore; Dipicolinic acid; DPA
ID GERMINATION MUTANTS; BACTERIAL-SPORES; SPORULATION; ENDOSPORES;
RESISTANCE; RADIATION; SEQUENCE; OPERON; SPOVA
AB Dipicolinic acid (pyridine-2,6-carboxylic acid; DPA) is a major component of bacterial spores and has been shown to be an important determinant of spore resistance. In the core of dormant Bacillus subtilis spores, DPA is associated with divalent calcium in a 1:1 chelate (Ca-DPA). Spores excrete Ca-DPA during germination, but it is unknown whether Ca and DPA are imported separately or together into the developing spore. Elemental analysis by scanning electron microscopy-energy-dispersive X-ray spectroscopy (SEM-EDS) of wild-type spores and mutant spores lacking the ability to synthesize DPA showed that DPA-less spores also lacked calcium, suggesting that the two compounds may be co-imported.
C1 [Nicholson, Wayne L.] Kennedy Space Ctr, Space Life Sci Lab, Gainesville, FL 32899 USA.
[Hintze, Paul E.] NASA, Corros Technol Lab, Gainesville, FL 32899 USA.
[Nicholson, Wayne L.] Univ Florida, Dept Microbiol & Cell Sci, Gainesville, FL 32899 USA.
RP Nicholson, WL (reprint author), Kennedy Space Ctr, Space Life Sci Lab, Bldg M6-1025 SLSL,Room 201-B, Gainesville, FL 32899 USA.
EM WLN@ufl.edu
OI Hintze, Paul/0000-0002-9962-2955
FU USDA [FLA-MCS-04602]
FX The authors wish to thank Pete Setlow for generous donation of the
strains used. This work was supported by USDA grant FLA-MCS-04602 to
W.L.N.
NR 25
TC 6
Z9 6
U1 0
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0302-8933
J9 ARCH MICROBIOL
JI Arch. Microbiol.
PD JUN
PY 2010
VL 192
IS 6
BP 493
EP 497
DI 10.1007/s00203-010-0569-5
PG 5
WC Microbiology
SC Microbiology
GA 597TT
UT WOS:000277785300009
PM 20396869
ER
PT J
AU Benford, J
Benford, G
Benford, D
AF Benford, James
Benford, Gregory
Benford, Dominic
TI Messaging with Cost-Optimized Interstellar Beacons
SO ASTROBIOLOGY
LA English
DT Article
DE SETI; METI; High-power microwaves; HPM; Microwave antennas
ID SEARCH
AB On Earth, how would we build galactic-scale beacons to attract the attention of extraterrestrials, as some have suggested we should do? From the point of view of expense to a builder on Earth, experience shows an optimum trade-off. This emerges by minimizing the cost of producing a desired power density at long range, which determines the maximum range of detectability of a transmitted signal. We derive general relations for cost-optimal aperture and power. For linear dependence of capital cost on transmitter power and antenna area, minimum capital cost occurs when the cost is equally divided between antenna gain and radiated power. For nonlinear power-law dependence, a similar simple division occurs. This is validated in cost data for many systems; industry uses this cost optimum as a rule of thumb. Costs of pulsed cost-efficient transmitters are estimated from these relations by using current cost parameters ($/W, $/m(2)) as a basis. We show the scaling and give examples of such beacons. Galactic-scale beacons can be built for a few billion dollars with our present technology. Such beacons have narrow "searchlight" beams and short "dwell times" when the beacon would be seen by an alien observer in their sky. More-powerful beacons are more efficient and have economies of scale: cost scales only linearly with range R, not as R(2), so number of stars radiated to increases as the square of cost. On a cost basis, they will likely transmit at higher microwave frequencies, similar to 10 GHz. The natural corridor to broadcast is along the galactic radius or along the local spiral galactic arm we are in. A companion paper asks "If someone like us were to produce a beacon, how should we look for it?"
C1 [Benford, James] Microwave Sci Inc, Lafayette, CA 94549 USA.
[Benford, Gregory] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Benford, Dominic] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Benford, J (reprint author), Microwave Sci Inc, Lafayette, CA 94549 USA.
EM jbenford@earthlink.net
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
NR 25
TC 12
Z9 12
U1 0
U2 6
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD JUN
PY 2010
VL 10
IS 5
BP 475
EP 490
DI 10.1089/ast.2009.0393
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 623WS
UT WOS:000279778100002
PM 20624056
ER
PT J
AU Benford, G
Benford, J
Benford, D
AF Benford, Gregory
Benford, James
Benford, Dominic
TI Searching for Cost-Optimized Interstellar Beacons
SO ASTROBIOLOGY
LA English
DT Article
DE SETI; METI; Microwave; Power beaming; Beacons; Radio astronomy; Array
antennas; High-power microwaves
ID EXTRATERRESTRIAL INTELLIGENCE; FOSSIL DIVERSITY; RADIO; SIGNALS; CYCLES;
SETI; WOW
AB What would SETI beacon transmitters be like if built by civilizations that had a variety of motives but cared about cost? In a companion paper, we presented how, for fixed power density in the far field, a cost-optimum interstellar beacon system could be built. Here, we consider how we should search for a beacon if it were produced by a civilization similar to ours. High-power transmitters could be built for a wide variety of motives other than the need for two-way communication; this would include beacons built to be seen over thousands of light-years. Extraterrestrial beacon builders would likely have to contend with economic pressures just as their terrestrial counterparts do. Cost, spectral lines near 1 GHz, and interstellar scintillation favor radiating frequencies substantially above the classic "water hole." Therefore, the transmission strategy for a distant, cost-conscious beacon would be a rapid scan of the galactic plane with the intent to cover the angular space. Such pulses would be infrequent events for the receiver. Such beacons built by distant, advanced, wealthy societies would have very different characteristics from what SETI researchers seek. Future searches should pay special attention to areas along the galactic disk where SETI searches have seen coherent signals that have not recurred on the limited listening time intervals we have used. We will need to wait for recurring events that may arrive in intermittent bursts. Several new SETI search strategies have emerged from these ideas. We propose a new test for beacons that is based on the Life Plane hypotheses.
C1 [Benford, James] Microwave Sci Inc, Lafayette, CA 94549 USA.
[Benford, Gregory] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Benford, Dominic] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
RP Benford, J (reprint author), Microwave Sci Inc, Lafayette, CA 94549 USA.
EM jbenford@earthlink.net
RI Benford, Dominic/D-4760-2012
OI Benford, Dominic/0000-0002-9884-4206
NR 34
TC 12
Z9 12
U1 0
U2 6
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD JUN
PY 2010
VL 10
IS 5
BP 491
EP 498
DI 10.1089/ast.2009.0394
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 623WS
UT WOS:000279778100003
PM 20624057
ER
PT J
AU Vaishampayan, P
Osman, S
Andersen, G
Venkateswaran, K
AF Vaishampayan, Parag
Osman, Shariff
Andersen, Gary
Venkateswaran, Kasthuri
TI High-Density 16S Microarray and Clone Library-Based Microbial Community
Composition of the Phoenix Spacecraft Assembly Clean Room
SO ASTROBIOLOGY
LA English
DT Article
DE Microbial ecology; Spacecraft assembly facility
ID MICROBIOLOGICAL PROFILES; DIVERSITY; ENVIRONMENTS; POPULATIONS; UNIFRAC;
DNA
AB The bacterial diversity and comparative community structure of a clean room used for assembling the Phoenix spacecraft was characterized throughout the spacecraft assembly process by using 16S rRNA gene cloning/sequencing and DNA microarray (PhyloChip) technologies. Samples were collected from several locations of the clean room at three time points: before Phoenix's arrival (PHX-B), during hardware assembly (PHX-D), and after the spacecraft was removed for launch (PHX-A). Bacterial diversity comprised of all major bacterial phyla of PHX-B was found to be statistically different from PHX-D and PHX-A samples. Due to stringent cleaning and decontamination protocols during assembly, PHX-D bacterial diversity was dramatically reduced when compared to PHX-B and PHX-A samples. Comparative community analysis based on PhyloChip results revealed similar overall trends as were seen in clone libraries, but the high-density phylogenetic microarray detected larger diversity in all sampling events. The decrease in community complexity in PHX-D compared to PHX-B, and the subsequent recurrence of these organisms in PHX-A, speaks to the effectiveness of NASA cleaning protocols. However, the persistence of a subset of bacterial signatures throughout all spacecraft assembly phases underscores the need for continued refinement of sterilization technologies and the implementation of safeguards that monitor and inventory microbial contaminants.
C1 [Vaishampayan, Parag; Venkateswaran, Kasthuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA USA.
[Osman, Shariff; Andersen, Gary] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Earth Sci, Dept Ecol, Berkeley, CA 94720 USA.
RP Vaishampayan, P (reprint author), 4800 Oak Grove Dr,M-S 89, Pasadena, CA 91109 USA.
EM vaishamp@jpl.nasa.gov
RI Andersen, Gary/G-2792-2015
OI Andersen, Gary/0000-0002-1618-9827
FU U.S. Department of Energy by the University of California, Lawrence
Berkeley National Laboratory (LBL) [DE-AC02-05CH11231]; NASA
FX Part of the research described in this publication was carried out at
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Additional work was performed under the auspices of the U.S. Department
of Energy by the University of California, Lawrence Berkeley National
Laboratory (LBL), under contract DE-AC02-05CH11231. This research was
funded by NASA Research Announcement (NRA) ROSS 2006 awarded to Kasthuri
Venkateswaran. We are grateful to members of the Biotechnology and
Planetary Protection group (JPL) and the Center for Environmental
Biotechnology (LBL) for technical assistance. We also appreciate the
help rendered by R. Sumner, B. Petsos, Y. Salinas, and D. Vaughn during
sampling, and T. DeSantis, E. Brodie, and Y. Piceno during PhyloChip
analysis. We are thankful to J. Spry, K. Buxbaum, C. Conley, and J.
Rummel for valuable advice and encouragement.
NR 42
TC 20
Z9 20
U1 0
U2 7
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD JUN
PY 2010
VL 10
IS 5
BP 499
EP 508
DI 10.1089/ast.2009.0443
PG 10
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 623WS
UT WOS:000279778100004
PM 20624058
ER
PT J
AU Lacy, CHS
Torres, G
Claret, A
Charbonneau, D
O'Donovan, FT
Mandushev, G
AF Lacy, Claud H. Sandberg
Torres, Guillermo
Claret, Antonio
Charbonneau, David
O'Donovan, Francis T.
Mandushev, Georgi
TI ABSOLUTE PROPERTIES OF THE ECLIPSING TRIPLE STAR CO ANDROMEDAE:
CONSTRAINTS ON CONVECTIVE CORE OVERSHOOTING
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; binaries: spectroscopic; stars: fundamental
parameters; stars: individual (CO And); stars: rotation; stars:
solar-type
ID LIMB-DARKENING COEFFICIENTS; SPECTROSCOPIC BINARIES; LIGHT CURVES; MODEL
ATMOSPHERES; TIDAL-EVOLUTION; Y-2 ISOCHRONES; STELLAR MODELS;
MAIN-SEQUENCE; TRANSFORMATIONS; TEMPERATURES
AB Accurate absolute properties have been determined for the eclipsing triple star CO And (F8+F8) based on extensive differential photometry obtained by three robotic observatories and CfA spectroscopy. The eclipsing binary star orbit is circular with a period of 3.655 days. The triple nature of this system is revealed by more than a century of timings of minimum light, and by the presence of third light in the photometric orbits. The masses of the eclipsing pair are 1.289 +/- 0.007 and 1.264 +/- 0.007 solar masses, and the corresponding radii are 1.727 +/- 0.021 and 1.694 +/- 0.017 solar radii. These stars are synchronously rotating and are near the end of their main-sequence phase, at an age of about 3.6 Gyr. The much fainter widely separated third body appears to have a mass of about 0.8 solar masses. The distance to the system is 377 +/- 25 pc.
C1 [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA.
[Torres, Guillermo; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[O'Donovan, Francis T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA.
RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA.
EM clacy@uark.edu; gtorres@cfa.harvard.edu; claret@iaa.es;
dcharbonneau@cfa.harvard.edu; ftod@caltech.edu; gmand@lowell.edu
RI O'Donovan, Francis/I-2423-2014;
OI O'Donovan, Francis/0000-0002-4858-6106; Charbonneau,
David/0000-0002-9003-484X
NR 79
TC 11
Z9 11
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2010
VL 139
IS 6
BP 2347
EP 2359
DI 10.1088/0004-6256/139/6/2347
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595WG
UT WOS:000277643700021
ER
PT J
AU Eisenhardt, PRM
Griffith, RL
Stern, D
Wright, EL
Ashby, MLN
Brodwin, M
Brown, MJI
Bussmann, RS
Dey, A
Ghez, AM
Glikman, E
Gonzalez, AH
Kirkpatrick, JD
Konopacky, Q
Mainzer, A
Vollbach, D
Wright, SA
AF Eisenhardt, Peter R. M.
Griffith, Roger L.
Stern, Daniel
Wright, Edward L.
Ashby, Matthew L. N.
Brodwin, Mark
Brown, Michael J. I.
Bussmann, R. S.
Dey, Arjun
Ghez, A. M.
Glikman, Eilat
Gonzalez, Anthony H.
Kirkpatrick, J. Davy
Konopacky, Quinn
Mainzer, Amy
Vollbach, David
Wright, Shelley A.
TI ULTRACOOL FIELD BROWN DWARF CANDIDATES SELECTED AT 4.5 mu m
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE brown dwarfs; infrared: galaxies; infrared: stars; stars: individual
(SDWFS J142831.46+354923.1; SDWFS J143524.44+335334.6; SDWFS
J143356.62+351849.2); stars: low-mass
ID ARRAY CAMERA IRAC; ADAPTIVE OPTICS SYSTEM; DUST-OBSCURED GALAXIES;
LONG-PERIOD VARIABLES; DIGITAL SKY SURVEY; T-DWARFS; MIDINFRARED
SELECTION; LOW-MASS; SPITZER; STARS
AB We have identified a sample of cool field brown dwarf candidates using IRAC data from the Spitzer Deep, Wide-Field Survey (SDWFS). The candidates were selected from 400,000 SDWFS sources with [4.5] <= 18.5 mag and were required to have [3.6] - [4.5] >= 1.5 and [4.5] - [8.0] <= 2.0 on the Vega system. The first color requirement selects objects redder than all but a handful of presently known brown dwarfs with spectral classes later than T7, while the second eliminates 14 probable reddened active galactic nuclei (AGNs). Optical detection of four of the remaining 18 sources implies they are likely also AGNs, leaving 14 brown dwarf candidates. For two of the brightest candidates (SDWFS J143524.44+335334.6 and SDWFS J143222.82+323746.5), the spectral energy distributions including near-infrared detections suggest a spectral class of similar to T8. The proper motion is <0 ''.25 yr(-1), consistent with expectations for a luminosity-inferred distance of >70 pc. The reddest brown dwarf candidate (SDWFS J143356.62+351849.2) has [3.6] - [4.5] = 2.24 and H - [4.5] > 5.7, redder than any published brown dwarf in these colors, and may be the first example of the elusive Y-dwarf spectral class. Models from Burrows et al. predict that larger numbers of cool brown dwarfs should be found for a Chabrier mass function. Suppressing the model [4.5] flux by a factor of 2, as indicated by previous work, brings the Burrows models and observations into reasonable agreement. The recently launched Wide-field Infrared Survey Explorer will probe a volume similar to 40x larger and should find hundreds of brown dwarfs cooler than T7.
C1 [Eisenhardt, Peter R. M.; Griffith, Roger L.; Stern, Daniel; Mainzer, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wright, Edward L.; Ghez, A. M.; Konopacky, Quinn] Univ Calif Los Angeles, Los Angeles, CA 90095 USA.
[Ashby, Matthew L. N.; Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Bussmann, R. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Glikman, Eilat] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Gonzalez, Anthony H.; Vollbach, David] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Kirkpatrick, J. Davy] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Wright, Shelley A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94709 USA.
RP Eisenhardt, PRM (reprint author), CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Peter.Eisenhardt@jpl.nasa.gov
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Wright, Shelley/0000-0003-1034-8054
FU National Optical Astronomy Observatory (NOAO); W. M. Keck Foundation;
NASA; National Science Foundation (NSF) [0708490]; NSF Science &
Technology Center; UCSC [AST-9876783]; Levine-Leichtman Family
Foundation
FX The authors thank Emanuele Daddi, Mark Dickinson, Jason Melbourne, and
Tom Soifer for assistance obtaining observations; Nick Seymour for
assistance with SDWFS and WIRC reductions; and Vandana Desai for the Mrk
231 spectrum and information about DOG SED's. Tom Soifer, Marcia Rieke,
Dan Weedman, and Jim Houck are thanked for allowing access to the GTO
MIPS survey of the NDWFS, and we acknowledge Buell Jannuzi's central
role in the NDWFS and related surveys of the field. Discussions with Roc
Cutri helped us understand the mid-IR characteristics of AGB stars, and
Szymon Kozlowski clarified questions about SDWFS variability
measurements. We thank the anonymous referee for a detailed and careful
review which improved the accuracy of the presentation. 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 contract with NASA. This work made use of images and
data products provided by the NOAO Deep Wide-Field Survey (NDWFS), which
is supported by the National Optical Astronomy Observatory (NOAO), and
follow-up NOAO surveys. NOAO is operated by AURA, Inc., under a
cooperative agreement with the National Science Foundation. Some of the
data presented herein were obtained at the W. M. Keck Observatory, which
is operated as a scientific partnership among Caltech, the University of
California and NASA. The Keck Observatory was made possible by the
generous financial support of the W. M. Keck Foundation, which also
provided support for M.B. Some data were obtained at the Hale Telescope,
Palomar Observatory as part of a continuing collaboration between
Caltech, NASA/JPL, and Cornell University. Support for this work was
provided by NASA through an award issued by JPL/Caltech. A.H.G.
acknowledges support for this work by the National Science Foundation
(NSF) under grant 0708490. Support for A.M.G. and Q.K.'s contribution to
this work was provided by the NSF Science & Technology Center for AO,
managed by UCSC (AST-9876783), and the Levine-Leichtman Family
Foundation.
NR 58
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2010
VL 139
IS 6
BP 2455
EP 2464
DI 10.1088/0004-6256/139/6/2455
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595WG
UT WOS:000277643700029
ER
PT J
AU Decin, L
De Beck, E
Brunken, S
Muller, HSP
Menten, KM
Kim, H
Willacy, K
de Koter, A
Wyrowski, F
AF Decin, L.
De Beck, E.
Bruenken, S.
Mueller, H. S. P.
Menten, K. M.
Kim, H.
Willacy, K.
de Koter, A.
Wyrowski, F.
TI Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri
II. In-depth non-LTE chemical abundance analysis
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; molecular processes; radiative transfer; submillimeter:
stars; stars: AGB and post-AGB; stars: mass-loss
ID MASS-LOSS RATES; SILICON ISOTOPIC ABUNDANCES; ROTATIONAL LINE-PROFILES;
GIANT BRANCH STARS; VY-CANIS MAJORIS; EVOLVED STARS; WATER-VAPOR;
EXPLOSIVE NUCLEOSYNTHESIS; COLLISIONAL EXCITATION; RADIATIVE-TRANSFER
AB Context. The interstellar medium is enriched primarily by matter ejected from evolved low and intermediate mass stars. The outflow from these stars creates a circumstellar envelope in which a rich gas-phase chemistry takes place. Complex shock-induced non-equilibrium chemistry takes place in the inner wind envelope, dust-gas reactions and ion-molecule reactions alter the abundances in the intermediate wind zone, and the penetration of cosmic rays and ultraviolet photons dissociates the molecules in the outer wind region.
Aims. Little observational information exists on the circumstellar molecular abundance stratifications of many molecules. Furthermore, our knowledge of oxygen-rich envelopes is not as profound as for the carbon-rich counterparts. The aim of this paper is therefore to study the circumstellar chemical abundance pattern of 11 molecules and isotopologs ((12)CO, (13)CO, SiS, (28)SiO, (29)SiO, (30)SiO, HCN, CN, CS, SO, SO(2)) in the oxygen-rich evolved star IK Tau.
Methods. We have performed an in-depth analysis of a large number of molecular emission lines excited in the circumstellar envelope around IK Tau. The analysis is done based on a non-local thermodynamic equilibrium (non-LTE) radiative transfer analysis, which calculates the temperature and velocity structure in a self-consistent way. The chemical abundance pattern is coupled to theoretical outer wind model predictions including photodestruction and cosmic ray ionization. Not only the integrated line intensities, but also the line shapes are used as diagnostic tool to study the envelope structure.
Results. The deduced wind acceleration is much slower than predicted from classical theories. SiO and SiS are depleted in the envelope, possibly due to the adsorption onto dust grains. For HCN and CS a clear difference with respect to inner wind non-equilibrium predictions is found, either indicating uncertainties in the inner wind theoretical modeling or the possibility that HCN and CS (or the radical CN) participate in the dust formation. The low signal-to-noise profiles of SO and CN prohibit an accurate abundance determination; the modeling of high-excitation SO2 lines is cumbersome, possibly related to line misidentifications or problems with the collisional rates. The SiO isotopic ratios ((29)SiO/(28)SiO and (30)SiO/ (28)SiO) point toward an enhancement in (28)SiO compared to results of classical stellar evolution codes. Predictions for H(2)O emission lines in the spectral range of the Herschel/HIFI mission are performed.
C1 [Decin, L.; De Beck, E.] Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, B-3001 Heverlee, Belgium.
[Decin, L.; de Koter, A.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekock, NL-1090 CE Amsterdam, Netherlands.
[Bruenken, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bruenken, S.; Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Mueller, H. S. P.; Menten, K. M.; Kim, H.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Kim, H.] MPI Gravitat Phy, D-30167 Hannover, Germany.
[Willacy, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands.
RP Decin, L (reprint author), Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, Celestijnenlaan 200D, B-3001 Heverlee, Belgium.
EM Leen.Decin@ster.kuleuven.ac.be
RI Brunken, Sandra/B-1880-2010;
OI Brunken, Sandra/0000-0001-7175-4828; Mueller, Holger/0000-0002-0183-8927
FU Fund for Scientific Research - Flanders (FWO) [G.0470.07];
Bundesministerium for Bildung und Forschung (BMBF)
FX We thank I. Cherchneff for useful discussion on the circumstellar non-TE
chemistry, and F. Schoier for providing us with an updated HCN linelist
in the LAMDA database. L.D. acknowledges financial support from the Fund
for Scientific Research - Flanders (FWO). E.D.B. acknowledges support
from the FWO under grant number G.0470.07. H.S.P.M. is very grateful to
the Bundesministerium for Bildung und Forschung (BMBF) for financial
support aimed at maintaining the Cologne Database for Molecular
Spectroscopy, CDMS. This support has been administered by the Deutsches
Zentrum fur Luft-und Raumfahrt (DLR). The computations for this research
have been done on the VIC HPC Cluster of the KULeuven. We are grateful
to the LUDIT HPC team for their support.
NR 92
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN-JUL
PY 2010
VL 516
AR A69
DI 10.1051/0004-6361/201014136
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 630LT
UT WOS:000280275400084
ER
PT J
AU Galametz, A
Stern, D
Stanford, SA
De Breuck, C
Vernet, J
Griffith, RL
Harrison, FA
AF Galametz, A.
Stern, D.
Stanford, S. A.
De Breuck, C.
Vernet, J.
Griffith, R. L.
Harrison, F. A.
TI Spectroscopic confirmation of a galaxy cluster associated with 7C
1756+6520 at z=1.416
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE large-scale structure of Universe; galaxies: clusters: general; Galaxy:
evolution; galaxies: individual: 7C 1756+6520; galaxies: clusters:
individual: 7C1756+6520
ID ACTIVE GALACTIC NUCLEI; IRAC SHALLOW SURVEY; YALE-CHILE MUSYC; RADIO
GALAXIES; X-RAY; MULTIWAVELENGTH SURVEY; MIDINFRARED SELECTION;
RED-SEQUENCE; PROTOCLUSTERS; TELESCOPE
AB We present spectroscopic follow-up of an overdensity of galaxies photometrically selected to be at 1.4 < z < 2.5 found in the vicinity of the radio galaxy 7C 1756+6520 at z = 1.4156. Using the DEIMOS optical multi-object spectrograph on the Keck 2 telescope, we observed a total of 129 BzK-selected sources, comprising 82 blue, star-forming galaxy candidates (sBzK) and 47 red, passively-evolving galaxy candidates (pBzK*), as well as 11 mid-infrared selected AGN candidates. We obtain robust spectroscopic redshifts for 36 blue galaxies, 7 red galaxies and 9 AGN candidates. Assuming all foreground interlopers were identified, we find that only 16% (9%) of the sBzK (pBzK*) galaxies are at z < 1.4. Therefore, the BzK criteria are shown to be relatively robust at identifying galaxies at moderate redshifts. Twenty-one galaxies, including the radio galaxy, four additional AGN candidates and three red galaxy candidates are found with 1.4156 +/- 0.025, forming a large scale structure at the redshift of the radio galaxy. Of these, eight have projected offsets < 2 Mpc relative to the radio galaxy position and have velocity offsets < 1000 km s(-1) relative to the radio galaxy redshift. This confirms that 7C 1756+6520 is associated with a high-redshift galaxy cluster. A second compact group of four galaxies is found at z similar to 1.437, forming a sub-group offset by Delta v similar to 3000 km s(-1) and approximately 1.'5 east of the radio galaxy.
C1 [Galametz, A.; De Breuck, C.; Vernet, J.] European So Observ, D-85748 Garching, Germany.
[Galametz, A.] Observ Astron, F-67000 Strasbourg, France.
[Stern, D.; Griffith, R. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
RP Galametz, A (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM agalamet@eso.org
OI Vernet, Joel/0000-0002-8639-8560; De Breuck, Carlos/0000-0002-6637-3315
FU NASA; US Department of Energy, National Nuclear Security Administration
[W-7405-Eng-48]
FX This work is based on a spectroscopic campaign at the W. M. Keck
Observatory, a scientific partnership between the University of
California and the California Institute of Technology, made possible by
a generous gift of the W. M. Keck Foundation. We are very grateful to
Tadayuki Kodama for having provided the models of red sequence presented
in this paper. We thank the anonymous referee for his/her careful
reading of the manuscript and constructive comments. The work of DS and
RLG was carried out at Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. S.A.S.'s work was performed
under the auspices of the US Department of Energy, National Nuclear
Security Administration by the University of California, Lawrence
Livermore National Laboratory under contract No. W-7405-Eng-48.
NR 37
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN-JUL
PY 2010
VL 516
AR A101
DI 10.1051/0004-6361/201014356
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 630LT
UT WOS:000280275400116
ER
PT J
AU Snodgrass, C
Meech, K
Hainaut, O
AF Snodgrass, C.
Meech, K.
Hainaut, O.
TI The nucleus of 103P/Hartley 2, target of the EPOXI mission
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: individual: 103P/Hartley 2
ID SPACE-TELESCOPE OBSERVATIONS; JUPITER-FAMILY COMETS; CCD PHOTOMETRY;
ENSEMBLE PROPERTIES; DISTANT COMETS
AB Context. 103P/Hartley 2 was selected as the target comet for the Deep Impact extended mission, EPOXI, in October 2007. There have been no direct optical observations of the nucleus of this comet, as it has always been highly active when previously observed.
Aims. We aimed to recover the comet near to aphelion, to: a) confirm that it had not broken up and was in the predicted position; b) to provide astrometry and brightness information for mission planning; and c) to continue the characterisation of the nucleus.
Methods. We observed the comet at heliocentric distances between 5.7 and 5.5 AU, using FORS2 at the VLT, at 4 epochs between May and July 2008. We performed VRI photometry on deep stacked images to look for activity and measure the absolute magnitude and therefore estimate the size of the nucleus.
Results. We recovered the comet near the expected position, with a magnitude of m(R) = 23.74 +/- 0.06 at the first epoch. The comet had no visible coma, although comparison of the profile with a stellar one showed that there was faint activity, or possibly a contribution to the flux from the dust trail from previous activity. This activity appears to fade at further epochs, implying that this is a continuation of activity past aphelion from the previous apparition rather than an early start to activity before the next perihelion. Our data imply a nucleus radius of <= 1 km for an assumed 4% albedo; we estimate a similar to 6% albedo. We measure a colour of (V - R) = 0.26 +/- 0.09.
C1 [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Snodgrass, C.] European So Observ, Casilla D, Chile.
[Meech, K.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Meech, K.] NASA, Astrobiol Inst, Washington, DC USA.
[Hainaut, O.] European So Observ, D-85748 Garching, Germany.
RP Snodgrass, C (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM snodgrass@mps.mpg.de
OI Snodgrass, Colin/0000-0001-9328-2905
FU EPOXI mission through University of Maryland [Z631506]
FX We thank ESO for awarding Director's Discretionary Time to this project,
the Paranal astronomers and telescope operators who performed the
observations for us and the referee, Dr. S. C. Lowry, for helpful
comments that improved this paper. This work is based in part on support
from the EPOXI mission through a subcontract from the University of
Maryland Z631506.
NR 16
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN-JUL
PY 2010
VL 516
AR L9
DI 10.1051/0004-6361/201014790
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 630LT
UT WOS:000280275400009
ER
PT J
AU de Martino, D
Falanga, M
Bonnet-Bidaud, JM
Belloni, T
Mouchet, M
Masetti, N
Andruchow, I
Cellone, SA
Mukai, K
Matt, G
AF de Martino, D.
Falanga, M.
Bonnet-Bidaud, J.-M.
Belloni, T.
Mouchet, M.
Masetti, N.
Andruchow, I.
Cellone, S. A.
Mukai, K.
Matt, G.
TI The intriguing nature of the high-energy gamma ray source XSS
J12270-4859
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: close; stars: individual: XSS J12270-4859; stars: individual:
1FGL J1227.9-4852; X-rays: binaries
ID XMM-NEWTON; CATACLYSMIC VARIABLES; LOW-MASS; VARIABILITY; BINARIES;
TELESCOPE; ACCRETION; CAMERA; IMAGER; STARS
AB Context. The nature of the hard X-ray source XSS J12270-4859 is still unclear. It was claimed to be a possible magnetic cataclysmic variable of the Intermediate Polar type from its optical spectrum and a possible 860 s X-ray periodicity in RXTE data. However, recent observations do not support the latter variability, leaving this X-ray source still unclassified.
Aims. To investigate its nature we present a broad-band X-ray and gamma ray study of this source based on a recent XMM-Newton observation and archival INTEGRAL and RXTE data. Using the Fermi/LAT 1-year point source catalogue, we tentatively associate XSS J12270-4859 with 1FGLJ1227.9-4852, a source of high-energy gamma rays with emission up to 10GeV. We further complement the study with UV photometry from XMM-Newton and ground-based optical and near-IR photometry.
Methods. We have analysed both timing and spectral properties in the gamma rays, X-rays, UV and optical/near-IR bands of XSS J12270-4859.
Results. The X-ray emission is highly variable, showing flares and intensity dips. The flares consist of flare-dip pairs. Flares are detected in both X-rays and the UV range, while the subsequent dips are present only in the X-ray band. Further aperiodic dipping behaviour is observed during X-ray quiescence, but not in the UV. The broad-band 0.2-100 keV X-ray/soft gamma ray spectrum is featureless and well described by a power law model with Gamma = 1.7. The high-energy spectrum from 100 MeV to 10 GeV is represented by a power law index of 2.45. The luminosity ratio between 0.1-100 GeV and 0.2-100 keV is similar to 0.8, indicating that the GeV emission is a significant component of the total energy output. Furthermore, the X-ray spectrum does not greatly change during flares, quiescence and the dips seen in quiescence. The X-ray spectrum however hardens during the post-flare dips, where a partial covering absorber is also required to fit the spectrum. Optical photometry acquired at different epochs reveals a period of 4.32 hr that could be ascribed to the binary orbital period. Near-IR, possibly ellipsoidal, variations are detected. Large amplitude variability on shorter (tens mins) timescales is found to be non-periodic.
Conclusions. The observed variability at all wavelengths together with the spectral characteristics strongly favour a low-mass atypical low-luminosity X-ray binary and are against a magnetic cataclysmic variable nature. The association with a Fermi/LAT high-energy gamma ray source further strengths this interpretation.
C1 [de Martino, D.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Falanga, M.] ISSI, CH-3012 Bern, Switzerland.
[Bonnet-Bidaud, J.-M.] CEA Saclay, DSM Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Belloni, T.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Mouchet, M.] Univ Paris 07, Lab APC, F-75005 Paris, France.
[Mouchet, M.] Observ Paris, LUTH, Sect Meudon, F-92195 Meudon, France.
[Masetti, N.] INAF Ist Astrofis Spaziale, I-40129 Bologna, Italy.
[Andruchow, I.; Cellone, S. A.] UNLP, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina.
[Andruchow, I.; Cellone, S. A.] CONICET UNLP, Inst Astrofis La Plata, La Plata, Buenos Aires, Argentina.
[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.
[Mukai, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Matt, G.] Univ Roma III, Dipartimento Fis, I-00146 Rome, Italy.
RP de Martino, D (reprint author), INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy.
EM demartino@oacn.inaf.it; mfalanga@issibern.ch; bonnetbidaud@cea.fr;
tomaso.belloni@brera.inaf.it; martine.mouchet@obspm.fr;
nicola.masetti@iasfbo.inaf.it; andru@fcaglp.fcaglp.unlp.edu.ar;
koji.mukai@nasa.gov; matt@fis.uniroma3.it
OI de Martino, Domitilla/0000-0002-5069-4202; Masetti,
Nicola/0000-0001-9487-7740
FU ASI [ASI/INAF I/023/05/06, ASI/INAF I/088/06/0]; INAF [PRIN-INAF 2007
N.17]
FX D.d.M., T. B. and N.M. acknowledge financial support from ASI under
contract ASI/INAF I/023/05/06 and ASI/INAF I/088/06/0 and also from INAF
under contract PRIN-INAF 2007 N.17. We gratefully acknowledge the help
of E. Bonning in the extraction of the counts map from the Fermi LAT
archive.
NR 36
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2010
VL 515
AR A25
DI 10.1051/0004-6361/200913802
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 606CN
UT WOS:000278399000025
ER
PT J
AU Doroshenko, V
Suchy, S
Santangelo, A
Staubert, R
Kreykenbohm, I
Rothschild, R
Pottschmidt, K
Wilms, J
AF Doroshenko, V.
Suchy, S.
Santangelo, A.
Staubert, R.
Kreykenbohm, I.
Rothschild, R.
Pottschmidt, K.
Wilms, J.
TI RXTE observations of the 1A 1118-61 in an outburst, and the discovery of
a cyclotron line
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; pulsars: individual: 1A 1118-61; binaries: general
ID X-RAY SOURCE
AB We present the analysis of RXTE monitoring data obtained during the 2009 January outburst of the hard X-ray transient 1A 1118-61. Using these observations the broadband (3.5-120 keV) spectrum of the source was measured for the first time ever. We have found that the broadband continuum spectrum of the source is similar to other accreting pulsars and is well described by several conventionally used phenomenological models. We have discovered that regardless of the applied continuum model, a prominent broad absorption feature at similar to 55 keV is observed. We interpret this feature as a cyclotron resonance scattering feature (CRSF). The observed CRSF energy is one of the highest known and corresponds to a magnetic field of B similar to 4.8 x 10(12) G in the scattering region. Our data also indicate the presence of an iron emission line presence that has not been previously reported for 1A 1118-61. Timing properties of the source, including a strong spin-up, were found to be similar to those observed by CGRO/BATSE during the previous outburst, but the broadband capabilities of RXTE reveal a more complicated energy dependency of the pulse-profile.
C1 [Doroshenko, V.; Santangelo, A.; Staubert, R.] Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Suchy, S.; Rothschild, R.] Univ Calif San Diego, CASS, La Jolla, CA 92093 USA.
[Kreykenbohm, I.; Wilms, J.] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Kreykenbohm, I.; Wilms, J.] Erlangen Ctr Astroparticle Phys ECAP, D-91058 Erlangen, Germany.
[Pottschmidt, K.] CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, K.] Univ Maryland Baltimore Cty, CSST, Baltimore, MD 21250 USA.
RP Doroshenko, V (reprint author), Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM doroshv@astro.uni-tuebingen.de
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013;
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
Doroshenko, Victor/0000-0001-8162-1105
FU DLR [50OR0702]
FX V.D. thanks DLR for financial support (grant 50OR0702).
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2010
VL 515
AR L1
DI 10.1051/0004-6361/201014858
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 633LS
UT WOS:000280505000003
ER
PT J
AU Dzyurkevich, N
Flock, M
Turner, NJ
Klahr, H
Henning, T
AF Dzyurkevich, N.
Flock, M.
Turner, N. J.
Klahr, H.
Henning, Th.
TI Trapping solids at the inner edge of the dead zone: 3-D global MHD
simulations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planets and satellites: formation; magnetohydrodynamics; methods:
numerical; instabilities; accretion, accretion disks; turbulence
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; TURBULENT PROTOPLANETARY
DISKS; ZERO NET FLUX; MAGNETOROTATIONAL INSTABILITY; ACCRETION DISKS;
SOLAR NEBULA; MAGNETIC-FIELDS; SHEARING BOX; PLANETESIMAL FORMATION;
FRACTIONAL IONIZATION
AB Context. The poorly-ionized interior of the protoplanetary disk or "dead zone" is the location where dust coagulation processes may be most efficient. However even here, planetesimal formation may be limited by the loss of solid material through radial drift, and by collisional fragmentation of the particles. Both depend on the turbulent properties of the gas.
Aims. Our aim here is to investigate the possibility that solid particles are trapped at local pressure maxima in the dynamically evolving disk. We perform the first 3-D global non-ideal magnetohydrodynamical (MHD) calculations of a section of the disk treating the turbulence driven by the magneto-rotational instability (MRI).
Methods. We use the ZeusMP code with a fixed Ohmic resistivity distribution. The domain contains an inner MRI-active region near the young star and an outer midplane dead zone, with the transition between the two modeled by a sharp increase in the magnetic diffusivity.
Results. The azimuthal magnetic fields generated in the active zone oscillate over time, changing sign about every 150 years. We thus observe the radial structure of the "butterfly pattern" seen previously in local shearing-box simulations. The mean magnetic field diffuses from the active zone into the dead zone, where the Reynolds stress nevertheless dominates, giving a residual a between 10(-4) and 10(-3). The greater total accretion stress in the active zone leads to a net reduction in the surface density, so that after 800 years an approximate steady state is reached in which a local radial maximum in the midplane pressure lies near the transition radius. We also observe the formation of density ridges within the active zone.
Conclusions. The dead zone in our models possesses a mean magnetic field, significant Reynolds stresses and a steady local pressure maximum at the inner edge, where the outward migration of planetary embryos and the efficient trapping of solid material are possible.
C1 [Dzyurkevich, N.; Flock, M.; Turner, N. J.; Klahr, H.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Turner, N. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dzyurkevich, N (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM natalia@mpia.de
FU Deutsches Zentrum fur Luft- und Raumfahrt (DLR); Deutsche
Forschungsgemeinschaft (DFG) through Forschergruppe [759]; The Formation
of Planets: The Critical First Growth Phase; NASA [07-SSO07-0044];
Alexander von Humboldt Foundation
FX N. Dzyurkevich acknowledges the support of the Deutsches Zentrum fur
Luft- und Raumfahrt (DLR). N. Dzyurkevich, M. Flock and H. Klahr were
supported in part by the Deutsche Forschungsgemeinschaft (DFG) through
Forschergruppe 759, "The Formation of Planets: The Critical First Growth
Phase". The participation of N. J. Turner was made possible by the NASA
Solar Systems Origins program under grant 07-SSO07-0044, and by the
Alexander von Humboldt Foundation through a Fellowship for Experienced
Researchers. The parallel computations were performed on the PIA cluster
of the Max Planck Institute for Astronomy Heidelberg, located at the
computing center of the Max Planck Society in Garching.
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2010
VL 515
AR A70
DI 10.1051/0004-6361/200912834
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 633LS
UT WOS:000280505000039
ER
PT J
AU Gielen, C
Van Wincke, H
Min, M
Waters, LBFM
Evans, TL
Matsuura, M
Deroo, P
Dominik, C
Reyniers, M
Zijlstra, A
Gordon, KD
Kemper, F
Indebetouw, R
Marengo, M
Meixner, M
Sloan, GC
Tielens, AGGM
Woods, PM
AF Gielen, C.
Van Wincke, H.
Min, M.
Waters, L. B. F. M.
Evans, T. Lloyd
Matsuura, M.
Deroo, P.
Dominik, C.
Reyniers, M.
Zijlstra, A.
Gordon, K. D.
Kemper, F.
Indebetouw, R.
Marengo, M.
Meixner, M.
Sloan, G. C.
Tielens, A. G. G. M.
Woods, P. M.
TI SPITZER-IRS spectral fitting of discs around binary post-AGB stars
Corrigendum
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: AGB and post-AGB; circumstellar matter;
binaries: general; Magellanic Clouds; errata, addenda
C1 [Gielen, C.; Van Wincke, H.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannckock, NL-1098 Amsterdam, Netherlands.
[Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Matsuura, M.] UCL, Dept Phys & Astron, UCL Inst Origins, London WC1E 6BT, England.
[Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, UCL Inst Origins, Dorking RH5 6NT, Surrey, England.
[Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Reyniers, M.] Royal Meteorol Inst Belgium, Dept Observat, B-1180 Brussels, Belgium.
[Zijlstra, A.; Kemper, F.; Woods, P. M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Gordon, K. D.; Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Tielens, A. G. G. M.] Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22906 USA.
[Min, M.] Univ Utrecht, Astron Inst Utrecht, NL-3584 CC Utrecht, Netherlands.
RP Gielen, C (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM clio.gielen@ster.kuleuven.be
FU Fund for Scientific Research of Flanders (FWO) [G.0178.02, G.0470.07];
NASA
FX C.G. and H.V.W. acknowledge support of the Fund for Scientific Research
of Flanders (FWO) under the grant G.0178.02. and G.0470.07. 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.
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SN 0004-6361
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JI Astron. Astrophys.
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PY 2010
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SC Astronomy & Astrophysics
GA 633LS
UT WOS:000280505000002
ER
PT J
AU Monin, JL
Guieu, S
Pinte, C
Rebull, L
Goldsmith, P
Fukagawa, M
Menard, F
Padgett, D
Stappelfeld, K
McCabe, C
Carey, S
Noriega-Crespo, A
Brooke, T
Huard, T
Terebey, S
Hillenbrand, L
Guedel, M
AF Monin, J. -L.
Guieu, S.
Pinte, C.
Rebull, L.
Goldsmith, P.
Fukagawa, M.
Menard, F.
Padgett, D.
Stappelfeld, K.
McCabe, C.
Carey, S.
Noriega-Crespo, A.
Brooke, T.
Huard, T.
Terebey, S.
Hillenbrand, L.
Guedel, M.
TI The large-scale disk fraction of brown dwarfs in the Taurus cloud as
measured with Spitzer
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; brown dwarfs; circumstellar matter; surveys; catalogs
ID INITIAL MASS FUNCTION; INFRARED ARRAY CAMERA; SPACE-TELESCOPE;
CHAMELEON-I; EVOLUTIONARY MODELS; CIRCUMSTELLAR DISK; STAR CLUSTER;
STELLAR; ATMOSPHERES; MEMBERS
AB Aims. The brown dwarf (BD) formation process has not yet been completely understood. To shed more light on the differences and similarities between star and BD formation processes, we study and compare the disk fraction among both kinds of objects over a large angular region in the Taurus cloud. In addition, we examine the spatial distribution of stars and BD relative to the underlying molecular gas.
Methods. In this paper, we present new and updated photometry data from the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope on 43 BDs in the Taurus cloud, and recalculate of the BD disk fraction in this region. We also useed recently available CO mm data to study the spatial distribution of stars and BDs relative to the cloud's molecular gas.
Results. We find that the disk fraction among BDs in the Taurus cloud is 41 +/- 12%, a value statistically consistent with the one among TTS (58 +/- 9%). We find that BDs in transition from a state where they have a disk to a diskless state are rare, and we study one isolated example of a transitional disk with an inner radius of approximate to 0.1 AU (CFHT BD Tau 12, found via its relatively small mid-IR excess compared to most members of Taurus that have disks. We find that BDs are statistically found in regions of similar molecular gas surface density to those associated with stars. Furthermore, we find that the gas column density distribution is almost identical for stellar and substellar objects with and without disks.
C1 [Monin, J. -L.; Menard, F.] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, F-38041 Grenoble, France.
[Guieu, S.; Rebull, L.; Padgett, D.; McCabe, C.; Carey, S.; Noriega-Crespo, A.; Brooke, T.] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Pinte, C.] Univ Exeter, Exeter EX4 4QL, Devon, England.
[Goldsmith, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fukagawa, M.] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Stappelfeld, K.; Hillenbrand, L.] CALTECH, Pasadena, CA 91125 USA.
[Brooke, T.] Univ Maryland, Baltimore, MD 21250 USA.
[Terebey, S.] Calif State Univ Los Angeles, Los Angeles, CA 90032 USA.
[Guedel, M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
RP Monin, JL (reprint author), Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, BP 53, F-38041 Grenoble, France.
EM Jean-Louis.Monin@obs.ujf-grenoble.fr
RI Guedel, Manuel/C-8486-2015;
OI Guedel, Manuel/0000-0001-9818-0588; Rebull, Luisa/0000-0001-6381-515X
FU CNRS/INSU, France
FX We thank an anonymous referee for a very detailed and precise report
that helped uncover several errors in the first version of this paper.
This research has made use of the CDS database. We thank the Programme
National de Physique Stellaire (PNPS, CNRS/INSU, France) for financial
support. The authors also wish to extend special thanks to those of
Hawaiian ancestry on whose sacred mountain of Mauna Kea we are
privileged to be guests. Without their generous hospitality, the CFH
Telescope observations presented therein would not have been possible.
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2010
VL 515
AR A91
DI 10.1051/0004-6361/200912338
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SC Astronomy & Astrophysics
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UT WOS:000280505000060
ER
PT J
AU Schmitz, F
Fleck, B
AF Schmitz, F.
Fleck, B.
TI Adiabatic high degree modes of a rotating star I. General features and
real pressure modes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE hydrodynamics; waves; stars: oscillations; Sun: oscillations; stars:
atmospheres
ID DIFFERENTIAL ROTATION; OSCILLATIONS; CHROMOSPHERE; STABILITY; FORM; SUN
AB Aims. The influence of the rotation of the Sun on non-radial p-modes with high wave numbers l is studied. To investigate and understand the basic properties of these modes, it is sufficient to consider only the outer layers of the Sun, which can be approximated by a plane layer with constant gravity.
Methods. We use a model with a smooth transition between a polytropic convection zone and an isothermal atmosphere. The rotation is simulated by a constant horizontal wind. For this model, using the column mass instead of the geometrical height, the adiabatic wave equation of the pressure perturbation can be reduced to Whittaker's differential equation. From boundary conditions we obtain the dispersion relation. The geometrical height is a simple elementary function of the column mass.
Results. The dispersion relation F(omega, k) = 0 is a higher order algebraic equation in both frequency and horizontal wave number, which must be solved numerically. We analyze the behavior of the dispersion curves of modes with an adiabatic exponent gamma = 5/3 for layers with polytropic indices n = 3 and n = 3/2. The f-mode is considered separately. For the understanding of the results we also consider modes of a homogeneous gas. We compare the k - omega diagram of our idealized model with the k - omega diagram of a real solar model.
C1 [Schmitz, F.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Fleck, B.] NASA, Goddard Space Flight Ctr, ESA Sci Operat Dept, Greenbelt, MD 20771 USA.
RP Schmitz, F (reprint author), Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
EM schmitz@astro.uni-wuerzburg.de; bfleck@esa.nascom.nasa.gov
RI Fleck, Bernhard/C-9520-2012
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
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SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2010
VL 515
AR A103
DI 10.1051/0004-6361/200912635
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SC Astronomy & Astrophysics
GA 633LS
UT WOS:000280505000072
ER
PT J
AU Shore, SN
Wahlgren, GM
AF Shore, S. N.
Wahlgren, G. M.
TI The O I] 1641 angstrom line as a probe of symbiotic star winds
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE binaries: symbiotic; atomic processes; galaxies: active; circumstellar
matter
ID ATOMIC OXYGEN; RS-OPHIUCHI; PARTIAL REDISTRIBUTION; RR-TELESCOPII; AG
DRACONIS; EMISSION; OUTBURST; SPECTRUM; TRANSITION; BINARY
AB The neutral oxygen resonance gimel 1302 angstrom line can, if the optical depth is sufficiently high, de-excite by an intercombination transition at gimel 1641 angstrom to a metastable state. This has been noted in a number of previous studies but never systematically investigated as a diagnostic of the neutral red giant wind in symbiotic stars and symbiotic-like recurrent novae. Methods. We used archival IUE high resolution, and HST GHRS and STIS medium and high resolution, spectra to study a sample of symbiotic stars. The integrated fluxes were measured, where possible, for the O I gimel 1302 angstrom and O I] lambda 1641 angstrom lines. Results. The intercombination lambda 1641 angstrom line is detected in a substantial number of symbiotic stars with optical depths that give column densities comparable with direct eclipse measures (EG And) and the evolution of the recurrent nova RS Oph 1985 in outburst. In four systems (EG And, Z And, V1016 Cyg, and RR Tel), we find that the O I] variations are strongly correlated with the optical light curve and outburst activity. This transition can also be important for the study of a wide variety of sources in which an ionization-bounded H II region is imbedded in an extensive neutral medium, including active galactic nuclei, and not only for evaluations of extinction.
C1 [Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, Pisa, Italy.
[Wahlgren, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wahlgren, G. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Shore, SN (reprint author), Univ Pisa, Dipartimento Fis Enrico Fermi, Largo B Pontecorvo 3, I-56127 Pisa, Italy.
EM shore@df.unipi.it
FU NASA [NNG06GJ29G]
FX We thank J. P. Aufdenberg, K. Genovali, J. Mikolajewska, C. Rossi, and
R. Viotti, and the (anonymous) referee for valuable discussions and
suggestions. The IUE and the HST GHRS and STIS spectra were obtained
from the MAST archive of STScI and archival visual photometric data were
provided by the AAVSO. G.M.W. acknowledges support from NASA Grant
NNG06GJ29G.
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JI Astron. Astrophys.
PD JUN
PY 2010
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DI 10.1051/0004-6361/201014271
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SC Astronomy & Astrophysics
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UT WOS:000280505000077
ER
PT J
AU Thompson, WT
AF Thompson, W. T.
TI Precision effects for solar image coordinates within the FITS world
coordinate system
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE standards; Sun: general; techniques: image processing; astronomical data
bases: miscellaneous; methods: data analysis
ID RADIO-EMISSION; REPRESENTATIONS; SCATTERING
AB The FITS world coordinate system (WCS) provides a number of tools for precisely specifying the spatial coordinates of an image. Many of the finer details that the WCS addresses have not historically been taken into account in solar image processing. This paper examines various effects which can affect the expression of coordinates in FITS headers, to determine under what conditions such effects need to be taken into account in data analysis, and under what conditions they can be safely ignored. Effects which are examined include perspective, parallax, spherical projection, optical axis determination, speed-of-light effects, stellar aberration, gravitational deflection, and scattering and refraction at radio wavelengths. Purely instrumental effects, such as misalignment or untreated optical aberrations, are not considered. Since the value of the solar radius is an experimental quantity, the effect of adopting a specific radius value is also examined. These effects are examined in the context of a previous paper outlining a WCS standard for encoding solar coordinates in FITS files. Aspects of that previous paper are clarified and extended in the present work.
C1 NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thompson, WT (reprint author), NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RI Thompson, William/D-7376-2012
FU NASA [NNG06EB68C]
FX The author would like to thank Dean Pesnell for many helpful
suggestions, and Gordon Holman and Jeffrey Brosius for useful references
on the theory of radio transport through a plasma. The author would also
like to thank the referee for many helpful comments and careful
criticisms. This work was carried out under NASA grant NNG06EB68C.
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JI Astron. Astrophys.
PD JUN
PY 2010
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SC Astronomy & Astrophysics
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UT WOS:000280505000028
ER
PT J
AU Bernat, D
Bouchez, AH
Ireland, M
Tuthill, P
Martinache, F
Angione, J
Burruss, RS
Cromer, JL
Dekany, RG
Guiwits, SR
Henning, JR
Hickey, J
Kibblewhite, E
McKenna, DL
Moore, AM
Petrie, HL
Roberts, J
Shelton, JC
Thicksten, RP
Trinh, T
Tripathi, R
Troy, M
Truong, T
Velur, V
Lloyd, JP
AF Bernat, David
Bouchez, Antonin H.
Ireland, Michael
Tuthill, Peter
Martinache, Frantz
Angione, John
Burruss, Rick S.
Cromer, John L.
Dekany, Richard G.
Guiwits, Stephen R.
Henning, John R.
Hickey, Jeff
Kibblewhite, Edward
McKenna, Daniel L.
Moore, Anna M.
Petrie, Harold L.
Roberts, Jennifer
Shelton, J. Chris
Thicksten, Robert P.
Trinh, Thang
Tripathi, Renu
Troy, Mitchell
Truong, Tuan
Velur, Viswa
Lloyd, James P.
TI A CLOSE COMPANION SEARCH AROUND L DWARFS USING APERTURE MASKING
INTERFEROMETRY AND PALOMAR LASER GUIDE STAR ADAPTIVE OPTICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; brown dwarfs; stars: low-mass; techniques: high
angular resolution
ID LOW-MASS STARS; BROWN DWARF; DYNAMICAL MASS; ULTRACOOL DWARFS;
BINARY-SYSTEMS; GJ 802B; MULTIPLICITY
AB We present a close companion search around 16 known early L dwarfs using aperture masking interferometry with Palomar laser guide star adaptive optics (LGS AO). The use of aperture masking allows the detection of close binaries, corresponding to projected physical separations of 0.6-10.0 AU for the targets of our survey. This survey achieved median contrast limits of Delta K similar to 2.3 for separations between 1.2 lambda/D-4 lambda/D and Delta K similar to 1.4 at 23 lambda/D. We present four candidate binaries detected with moderate-to- high confidence (90%-98%). Two have projected physical separations less than 1.5 AU. This may indicate that tight-separation binaries contribute more significantly to the binary fraction than currently assumed, consistent with spectroscopic and photometric overluminosity studies. Ten targets of this survey have previously been observed with the Hubble Space Telescope as part of companion searches. We use the increased resolution of aperture masking to search for close or dim companions that would be obscured by full aperture imaging, finding two candidate binaries. This survey is the first application of aperture masking with LGS AO at Palomar. Several new techniques for the analysis of aperture masking data in the low signal-to-noise regime are explored.
C1 [Bernat, David; Lloyd, James P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Henning, John R.; Hickey, Jeff; McKenna, Daniel L.; Petrie, Harold L.; Thicksten, Robert P.; Tripathi, Renu] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Bouchez, Antonin H.; Angione, John; Burruss, Rick S.; Cromer, John L.; Dekany, Richard G.; Guiwits, Stephen R.; Henning, John R.; Hickey, Jeff; Kibblewhite, Edward; McKenna, Daniel L.; Moore, Anna M.; Petrie, Harold L.; Roberts, Jennifer; Shelton, J. Chris; Thicksten, Robert P.; Trinh, Thang; Tripathi, Renu; Troy, Mitchell; Truong, Tuan; Velur, Viswa] CALTECH, Palomar Observ, Palomar Laser Guide Star Adapt Opt Team, Palomar Mt, CA 92060 USA.
[Ireland, Michael; Tuthill, Peter] Univ Sydney, Sch Phys, Sydney Inst Astrophys, Sydney, NSW 2006, Australia.
[Martinache, Frantz] Natl Inst Nat Sci, Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Angione, John; Burruss, Rick S.; Guiwits, Stephen R.; Roberts, Jennifer; Shelton, J. Chris; Trinh, Thang; Troy, Mitchell; Truong, Tuan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kibblewhite, Edward] Univ Chicago, Chicago, IL 60637 USA.
RP Bernat, D (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RI Lloyd, James/B-3769-2011;
OI Ireland, Michael/0000-0002-6194-043X
FU National Science Foundation [AST-0905932, AST-0705085]; National
Aeronautics and Space Administration
FX We thank the staff and telescope operators of the Palomar Observatory
for their support. David Bernat thanks Jason Wright for many helpful
discussions about the analytical techniques developed within this paper.
We thank the Palomar staff for many nights of assistance at the Palomar
Hale telescope. This work was supported in part by the National Science
Foundation under award numbers AST-0905932 and AST-0705085. The Hale
telescope at Palomar Observatory is operated as part of a collaborative
agreement between Caltech, JPL, and Cornell University. 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, and
is funded by the National Aeronautics and Space Administration, and the
National Science Foundation.
NR 30
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 724
EP 735
DI 10.1088/0004-637X/715/2/724
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100001
ER
PT J
AU Sandell, G
Wright, M
AF Sandell, Goeran
Wright, Melvyn
TI A DETAILED STUDY OF THE ACCRETION DISK SURROUNDING THE HIGH-MASS
PROTOSTAR NGC 7538 S
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: clouds; stars: formation; stars: pre-main
sequence; submillimeter: stars
ID YOUNG STELLAR OBJECTS; (PROTO)STAR IRAS 20126+4104; HYPERCOMPACT
HII-REGIONS; VELOCITY MOLECULAR GAS; T-TAURI STARS; METHANOL MASERS;
NGC-7538 REGION; ROTATING TOROIDS; HYDROXYL MASERS; HIGH-RESOLUTION
AB We present deep high-angular resolution observations of the high-mass protostar NGC 7538 S, which is in the center of a cold dense cloud core with a radius of 0.5 pc and a mass of similar to 2000 M(circle dot). These observations show that NGC 7538 S is embedded in a compact elliptical core with a mass of 85-115 M(circle dot). The star is surrounded by a rotating accretion disk, which powers a very young, hot molecular outflow approximately perpendicular to the rotating accretion disk. The accretion rate is very high, similar to(1.4-2.8) x 10(-3) M(circle dot) yr(-1). Evidence for rotation of the disk surrounding the star is seen in all largely optically thin molecular tracers, H(13)CN J = 1 -> 0, HN(13)C J = 1 -> 0, H(13)CO(+) J = 1 -> 0, and DCN J = 3 -> 2. Many molecules appear to be affected by the hot molecular outflow, including DCN and H(13)CO(+). The emission from CH(3)CN, which has often been used to trace disk rotation in young high-mass stars, is dominated by the outflow, especially at higher K levels. Our new high angular resolution observations show that the rotationally supported part of the disk is smaller than we previously estimated. The enclosed mass of the inner, rotationally supported part of the disk (D similar to 5 '', i.e., 14,000 AU) is similar to 14-24M(circle dot).
C1 [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
RP Sandell, G (reprint author), NASA, Ames Res Ctr, SOFIA USRA, MS N211-3, Moffett Field, CA 94035 USA.
EM Goran.H.Sandell@nasa.gov
FU National Science Foundation
FX The BIMA array was operated by the Universities of California
(Berkeley), Illinois, and Maryland with support from the National
Science Foundation. We want to thank Dr. W.M. Goss for helpful comments
and support throughout this project. Special thanks goes to Dr. Mark
Heyer, who did the FCRAO observations for us, and to the JCMT telescope
system specialists, who did all the JCMT observing in service mode. We
thank the anonymous referee for an extremely careful reading of our
paper, which considerably improved it.
NR 79
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U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 919
EP 938
DI 10.1088/0004-637X/715/2/919
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100017
ER
PT J
AU Torrejon, JM
Schulz, NS
Nowak, MA
Kallman, TR
AF Torrejon, J. M.
Schulz, N. S.
Nowak, M. A.
Kallman, T. R.
TI A CHANDRA SURVEY OF FLUORESCENCE Fe LINES IN X-RAY BINARIES AT HIGH
RESOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (X1908+075); surveys; X-rays: binaries
ID IRON LINE; EMISSION-LINES; STELLAR WIND; INTERSTELLAR-MEDIUM; COMPTON
SHOULDER; ACCRETION DISKS; BLACK-HOLE; CYGNUS X-1; VELA X-1; K-LINES
AB Fe K line fluorescence is commonly observed in the X-ray spectra of many X-ray binaries (XRBs) and represents a fundamental tool to investigate the material surrounding the X-ray source. In this paper, we present a comprehensive survey of 41 XRBs (10 HMXBs and 31 LMXBs) with Chandra with specific emphasis on the Fe K region and the narrow Fe K alpha line, at the highest resolution possible. We find that (1) the Fe K alpha line is always centered at lambda = 1.9387 +/- 0.0016 angstrom, compatible with Fe I up to Fe x; we detect no shifts to higher ionization states nor any difference between high mass X-ray binaries (HMXBs) and low mass X-ray binaries (LMXBs). (2) The line is very narrow, with FWHM < 5 m angstrom, normally not resolved by Chandra which means that the reprocessing material is not rotating at high speeds. (3) Fe K alpha fluorescence is present in all the HMXBs in the survey. In contrast, such emissions are astonishingly rare (similar to 10%) among LMXBs where only a few out of a large number showed Fe K fluorescence. However, the line and edge properties of these few are very similar to their high mass cousins. (4) The lack of Fe line emission is always accompanied by the lack of any detectable K edge. (5) We obtain the empirical curve of growth of the equivalent width of the Fe K alpha line versus the density column of the reprocessing material, i.e., EW(K alpha) versus N(H), and show that it is consistent with a reprocessing region spherically distributed around the compact object. (6) We show that fluorescence in XRBs follows the X-ray Baldwin effect as previously only found in the X-ray spectra of active galactic nuclei. We interpret this finding as evidence of decreasing neutral Fe abundance with increasing X-ray illumination and use it to explain some spectral states of Cyg X-1 as a possible cause of the lack of narrow Fe line emission in LMXBs. (7) Finally, we study anomalous morphologies such as Compton shoulders and asymmetric line profiles associated with the line fluorescence. Specifically, we present the first evidence of a Compton shoulder in the HMXB X1908+075. Also, the Fe K alpha lines of 4U1700-37 and LMC X-4 present asymmetric wings, suggesting the presence of highly structured stellar winds in these systems.
C1 [Torrejon, J. M.] Univ Alicante, Inst Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain.
[Torrejon, J. M.; Schulz, N. S.; Nowak, M. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Torrejon, JM (reprint author), Univ Alicante, Inst Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain.
EM jmt@ua.es
RI Torrejon, Jose /K-6395-2014
OI Torrejon, Jose /0000-0002-5967-5163
FU Spanish Ministerio de Educacion y Ciencia (MEC) [PR2007-0176]; MICINN
[AYA2008-06166-C03-03, CSD-2006-00070]
FX We thank Julia Lee for making the LMC X-4 data available to us previous
to publication. J.M.T. acknowledges the support of the Spanish
Ministerio de Educacion y Ciencia (MEC) through the grant PR2007-0176,
and the MICINN through grants AYA2008-06166-C03-03 and Consolider-GTC
CSD-2006-00070.
NR 40
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 947
EP 958
DI 10.1088/0004-637X/715/2/947
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100019
ER
PT J
AU Ostorero, L
Moderski, R
Stawarz, L
Diaferio, A
Kowalska, I
Cheung, CC
Kataoka, J
Begelman, MC
Wagner, SJ
AF Ostorero, L.
Moderski, R.
Stawarz, L.
Diaferio, A.
Kowalska, I.
Cheung, C. C.
Kataoka, J.
Begelman, M. C.
Wagner, S. J.
TI X-RAY-EMITTING GHz-PEAKED-SPECTRUM GALAXIES: TESTING A
DYNAMICAL-RADIATIVE MODEL WITH BROADBAND SPECTRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (IERS B0026+346, IERS B0108+388,
IERS B0500+019, IERS B0710+439, PKS B0941-080, IERS B1031+567, IERS
B1345+125, IVS B1358+624, IERS B1404+286, IERS B2128+048, IERS
B2352+495); galaxies: jets; radiation mechanisms: non-thermal; X-rays:
galaxies
ID COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; POWERFUL RADIO GALAXIES;
ULTRALUMINOUS INFRARED GALAXIES; SPITZER-SPACE-TELESCOPE;
PEARSON-READHEAD SURVEY; HIGH-FREQUENCY PEAKERS; FREE-FREE ABSORPTION;
NARROW-LINE REGION; MULTIBAND IMAGING PHOTOMETER
AB In a dynamical-radiative model we recently developed to describe the physics of compact, GHz-peaked-spectrum (GPS) sources, the relativistic jets propagate across the inner, kpc-sized region of the host galaxy, while the electron population of the expanding lobes evolves and emits synchrotron and inverse-Compton (IC) radiation. Interstellarmedium gas clouds engulfed by the expanding lobes, and photoionized by the active nucleus, are responsible for the radio spectral turnover through free-free absorption (FFA) of the synchrotron photons. The model provides a description of the evolution of the spectral energy distribution (SED) of GPS sources with their expansion, predicting significant and complex high-energy emission, from the X-ray to the gamma-ray frequency domain. Here, we test this model with the broadband SEDs of a sample of 11 X-ray-emitting GPS galaxies with compact-symmetric-object morphology, and show that (1) the shape of the radio continuum at frequencies lower than the spectral turnover is indeed well accounted for by the FFA mechanism and (2) the observed X-ray spectra can be interpreted as non-thermal radiation produced via IC scattering of the local radiation fields off the lobe particles, providing a viable alternative to the thermal, accretion-disk-dominated scenario. We also show that the relation between the hydrogen column densities derived from the X-ray (NH) and radio (NHi) data of the sources is suggestive of a positive correlation, which, if confirmed by future observations, would provide further support to our scenario of high-energy emitting lobes.
C1 [Ostorero, L.; Diaferio, A.] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Ostorero, L.; Diaferio, A.] Ist Nazl Fis Nucl, I-10125 Turin, Italy.
[Moderski, R.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Moderski, R.; Stawarz, L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Kowalska, I.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Cheung, C. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Begelman, M. C.] Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA.
[Wagner, S. J.] Landessternwarte Heidelberg Konigstuhl, D-69117 Heidelberg, Germany.
RP Ostorero, L (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy.
OI Ostorero, Luisa/0000-0003-3983-5980
NR 212
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U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1071
EP 1093
DI 10.1088/0004-637X/715/2/1071
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100029
ER
PT J
AU Burrows, RH
Zank, GP
Webb, GM
Burlaga, LF
Ness, NF
AF Burrows, R. H.
Zank, G. P.
Webb, G. M.
Burlaga, L. F.
Ness, N. F.
TI PICKUP ION DYNAMICS AT THE HELIOSPHERIC TERMINATION SHOCK OBSERVED BY
VOYAGER 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; shock waves; Sun: heliosphere
ID SOLAR-WIND; PERPENDICULAR SHOCKS; ACCELERATION; MICROSTRUCTURE
AB The recent Voyager 2 (V2) observations of the termination shock (TS) indicate that it is a plasma shock unlike any other in the heliosphere with the dynamics and structure heavily influenced by the presence of an energized population of pickup ions (PUIs). The "unexpected" finding of cold plasma downstream of the TS in the heliosheath, corresponding to very little heating of the thermal solar wind (SW), suggests that the energy dissipated by the shock is dominated by the energization of PUIs at the TS. We examine the "shock surfing" mechanism at the test particle level, where multiply reflected ions (MRIs) gain energy from the motional electric field as a consequence of reflection from the cross-shock potential (CSP), for a model of the TS3 (the third TS crossing measured by V2). The energization of PUI filled-shell distributions at a stationary, perpendicular model of the TS3 indicates that shock surfing can provide both substantial PUI acceleration and a dissipation mechanism at the TS. For a sufficiently strong CSP and sufficiently narrow shock ramp MRI acceleration can account for the "missing" energy of the downstream SW plasma.
C1 [Burrows, R. H.; Zank, G. P.; Webb, G. M.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ness, N. F.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Burrows, RH (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
FU NASA [NNX09AB40G, NNX07AH18G, NNG05EC85C, NNX09 AG63G, NNX08AJ21G,
NNX09AB24G, NNX09AG29G, NNX09AG62G]
FX We acknowledge the partial support of NASA grants NNX09AB40G,
NNX07AH18G, NNG05EC85C, NNX09 AG63G, NNX08AJ21G, NNX09AB24G, NNX09AG29G,
and NNX09AG62G.
NR 20
TC 20
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1109
EP 1116
DI 10.1088/0004-637X/715/2/1109
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100031
ER
PT J
AU Paganini, L
Villanueva, GL
Lara, LM
Lin, ZY
Kuppers, M
Hartogh, P
Faure, A
AF Paganini, L.
Villanueva, G. L.
Lara, L. M.
Lin, Z. Y.
Kueppers, M.
Hartogh, P.
Faure, A.
TI HCN SPECTROSCOPY OF COMET 73P/SCHWASSMANN-WACHMANN 3. A STUDY OF GAS
EVOLUTION AND ITS LINK TO CN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; comets: individual
(73P/Schwassmann-Wachmann 3); molecular processes; radiative transfer
ID BOPP 1995 O1; HALE-BOPP; EXCITATION CONDITIONS; VOLATILE COMPOSITION;
RADIATIVE-TRANSFER; HYDROGEN-CYANIDE; FRAGMENT-B; INNER COMA; C/1996 B2;
WATER
AB In 2006 May, comet 73P/Schwassmann-Wachmann 3 experienced large outburst activity allowing us to study the gas production rate of fresh material released from the nucleus. We observed the comet in a coordinated campaign using millimeter and optical facilities at heliocentric distances between 0.966 and 1.033 AU. During this time, we had the opportunity to follow the post-outburst evolution of fragment B, which evidenced larger production rates in comparison to fragment C, the latter showing a rather stable gas production rate (Q(HCN) similar to 2 x 10(25) molecules s(-1)). In addition to the investigation of the gas evolution, we studied the possible role of HCN and dust as progenitors for the CN radical. From our joint observations on May 12, we observed a high correlation of CN with HCN and low correlation with the continuum emission (grains). Herewith, our study supports the view of HCN as a major source of CN, although the presence of other sources for cyanide cannot be fully ruled out.
C1 [Paganini, L.; Villanueva, G. L.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Paganini, L.; Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Lara, L. M.; Lin, Z. Y.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
[Kueppers, M.] ESAC, Madrid 28691, Spain.
[Faure, A.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble LAOG, F-38041 Grenoble 09, France.
RP Paganini, L (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 693-0, Greenbelt, MD 20771 USA.
EM lucas.paganini@nasa.gov
FU Max-Planck-Gesellschaft; Spanish Ministerio de Educacion y Ciencia;
Ministerio de Ciencia e Innovacion [ESP2006-02934, AyA 2009-08011]
FX This work is based on joint observations from the Heinrich Hertz
Submillimeter Telescope and Lulin Observatory. We are grateful to the
staff of HHSMT and LO for their great assistance and generous allocation
of telescope time throughout our observational campaign. L. P.
acknowledges D. Bockelee-Morvan, N. Biver, K. Jockers, M. Drahus, M.
Lippi, and M.J. Mumma for useful discussions, the anonymous referee for
valuable comments on the manuscript, and the support of this research by
the Max-Planck-Gesellschaft. L. M. L. and Z.-Y.L. thank the support
given by the Spanish Ministerio de Educacion y Ciencia and Ministerio de
Ciencia e Innovacion under projects ESP2006-02934 and AyA 2009-08011.
The SMT is operated by the Arizona Radio Observatory (ARO), Steward
Observatory, University of Arizona.
NR 57
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U1 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1258
EP 1269
DI 10.1088/0004-637X/715/2/1258
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100042
ER
PT J
AU Goldsmith, PF
Velusamy, T
Li, D
Langer, WD
AF Goldsmith, Paul F.
Velusamy, Thangasamy
Li, Di
Langer, William D.
TI MOLECULAR HYDROGEN EMISSION FROM THE BOUNDARIES OF THE TAURUS MOLECULAR
CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (Taurus molecular cloud); ISM:
molecules; photon-dominated region (PDR)
ID POLYCYCLIC AROMATIC-HYDROCARBON; WARM NEUTRAL HALOS; H-I; H-2 EMISSION;
DARK CLOUDS; GAS; CO; PHOTODISSOCIATION; CHEMISTRY; REGIONS
AB We report Spitzer Space Telescope observations of the four lowest rotational transitions of H(2) in three portions of the boundary of the Taurus molecular cloud. Emission in the two lowest transitions, S(0) and S(1), was detected in almost all pointing directions, while the S(2) and S(3) lines were marginally detected only after further averaging of data. The widespread detection of lines coming from levels 510 K and 1016 K above the molecular ground state is indicative of gas at a temperature of at least 200 K containing column densities (1-5) x 10(18) cm(-2) of H(2). For the region with the simplest geometry, we have used the Meudon PDR code to model the chemistry, radiative transfer, and excitation of molecular hydrogen. We conclude that models with acceptable values of the UV interstellar radiation field can reproduce the amount of H(2) in the lowest excited state, but cannot account for the degree of excitation of the H(2). The unexpectedly high degree of excitation of the H(2) in the boundary layer of a molecular cloud, which cannot be explained by the presence of stellar sources, points to an enhanced heating rate which may be the result of, e. g., dissipation of turbulence. We have in one boundary region been able to obtain the ortho-to-para ratio (OPR) for H(2), which by modeling and possible detection of the S(2) and S(3) lines has a range 1.0 >= OPR >= 0.15, although this result must be treated with caution. The fact that the ortho-to-para ratio is lower than that expected for equilibrium at the gas kinetic temperature may be indicative of circulation of material from cold, purely molecular regions into the boundary layer, possibly due to turbulent diffusion. The explanation of these data may thus be suggestive of processes that are having a significant effect on the structure and evolution of molecular clouds and the star formation that takes place within them.
C1 [Goldsmith, Paul F.; Velusamy, Thangasamy; Li, Di; Langer, William D.] Jet Prop Lab, Pasadena, CA 91103 USA.
RP Goldsmith, PF (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91103 USA.
EM Paul.F.Goldsmith@jpl.nasa.gov
RI Goldsmith, Paul/H-3159-2016
FU Jet Propulsion Laboratory, California Institute of Technology
FX This work was supported in part by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. We thank the Spitzer Science
Center for hosting an enjoyable stay during which P. F. G. was able to
make substantial progress on this research. We are very grateful to
Franck Le Petit for his support in using the Meudon PDR code and
answering numerous questions about details of its operation. We thank
David Neufeld for discussions about the H2 molecule and David
Hollenbach for valuable comments about UV pumping of H2, as
well as numerous other suggestions that materially improved this paper.
We are grateful to Luisa Rebull, Debbie Padgett, and Helen Kirk for
providing critical information about the B stars associated with Taurus.
We thank Bill Reach for sharing information about the stellar population
and radiation field limits in Taurus, and Darek Lis for discussions
about observations of PDR regions. We appreciate substantial work by
Jorge Pineda to compare results of various PDR codes and the very
helpful comments of an anonymous referee. This research has made use of
NASA's Astrophysics Data System and of the SIMBAD database, operated at
CDS, Strasbourg, France.
NR 37
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U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1370
EP 1382
DI 10.1088/0004-637X/715/2/1370
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100052
ER
PT J
AU Ahn, HS
Allison, PS
Bagliesi, MG
Barbier, L
Beatty, JJ
Bigongiari, G
Brandt, TJ
Childers, JT
Conklin, NB
Coutu, S
DuVernois, MA
Ganel, O
Han, JH
Jeon, JA
Kim, KC
Lee, J
Lee, MH
Maestro, P
Malinin, A
Marrocchesi, PS
Minnick, S
Mognet, SI
Na, GW
Nam, J
Nam, S
Nutter, S
Park, IH
Park, NH
Seo, ES
Sina, R
Walpole, P
Wu, J
Yang, J
Yoon, YS
Zei, R
Zinn, SY
AF Ahn, H. S.
Allison, P. S.
Bagliesi, M. G.
Barbier, L.
Beatty, J. J.
Bigongiari, G.
Brandt, T. J.
Childers, J. T.
Conklin, N. B.
Coutu, S.
DuVernois, M. A.
Ganel, O.
Han, J. H.
Jeon, J. A.
Kim, K. C.
Lee, J.
Lee, M. H.
Maestro, P.
Malinin, A.
Marrocchesi, P. S.
Minnick, S.
Mognet, S. I.
Na, G. W.
Nam, J.
Nam, S.
Nutter, S.
Park, I. H.
Park, N. H.
Seo, E. S.
Sina, R.
Walpole, P.
Wu, J.
Yang, J.
Yoon, Y. S.
Zei, R.
Zinn, S. Y.
TI MEASUREMENTS OF THE RELATIVE ABUNDANCES OF HIGH-ENERGY COSMIC-RAY NUCLEI
IN THE TeV/NUCLEON REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; balloons; diffusion; Galaxy: abundances
ID SILICON CHARGE DETECTOR; CREAM EXPERIMENT; CROSS-SECTIONS; 1ST FLIGHT;
SPECTRA; ELEMENTS; PROPAGATION; SECONDARY; TRANSPORT; HYDROGEN
AB We present measurements of the relative abundances of cosmic-ray nuclei in the energy range of 500-3980 GeV/nucleon from the second flight of the Cosmic Ray Energetics And Mass balloon-borne experiment. Particle energy was determined using a sampling tungsten/scintillating-fiber calorimeter, while particle charge was identified precisely with a dual-layer silicon charge detector installed for this flight. The resulting element ratios C/O, N/O, Ne/O, Mg/O, Si/O, and Fe/O at the top of atmosphere are 0.919 +/- 0.123(stat) +/- 0.030(syst), 0.076 +/- 0.019(stat) +/- 0.013(syst), 0.115 +/- 0.031(stat) +/- 0.004(syst), 0.153 +/- 0.039(stat) +/- 0.005(syst), 0.180 +/- 0.045(stat) +/- 0.006(syst), and 0.139 +/- 0.043(stat) +/- 0.005(syst), respectively, which agree with measurements at lower energies. The source abundance of N/O is found to be 0.054 +/- 0.013(stat) +/- 0.009(-0.017)(syst+0.010esc). The cosmic-ray source abundances are compared to local Galactic (LG) abundances as a function of first ionization potential and as a function of condensation temperature. At high energies the trend that the cosmic-ray source abundances at large ionization potential or low condensation temperature are suppressed compared to their LG abundances continues. Therefore, the injection mechanism must be the same at TeV/nucleon energies as at the lower energies measured by HEAO-3, CRN, and TRACER. Furthermore, the cosmic-ray source abundances are compared to a mixture of 80% solar system abundances and 20% massive stellar outflow (MSO) as a function of atomic mass. The good agreement with TIGER measurements at lower energies confirms the existence of a substantial fraction of MSO material required in the similar to TeV per nucleon region.
C1 [Jeon, J. A.; Na, G. W.; Nam, J.; Nam, S.; Park, I. H.; Park, N. H.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
[Ahn, H. S.; Ganel, O.; Han, J. H.; Kim, K. C.; Lee, M. H.; Malinin, A.; Seo, E. S.; Sina, R.; Walpole, P.; Wu, J.; Yoon, Y. S.; Zinn, S. Y.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Allison, P. S.; Beatty, J. J.; Brandt, T. J.; Yoon, Y. S.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Bagliesi, M. G.; Bigongiari, G.; Maestro, P.; Marrocchesi, P. S.; Zei, R.] Univ Siena, Dept Phys, I-53100 Siena, Italy.
[Bagliesi, M. G.; Bigongiari, G.; Maestro, P.; Marrocchesi, P. S.; Zei, R.] Ist Nazl Fis Nucl, I-53100 Siena, Italy.
[Barbier, L.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Childers, J. T.; DuVernois, M. A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Conklin, N. B.; Coutu, S.; Mognet, S. I.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Minnick, S.] Kent State Univ, Dept Phys, New Philadelphia, OH 44663 USA.
[Nutter, S.] Univ Kentucky, Dept Phys & Geol, Highland Hts, KY 41099 USA.
[Seo, E. S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Park, IH (reprint author), Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
EM ipark@ewha.ac.kr
RI maestro, paolo/E-3280-2010; Beatty, James/D-9310-2011; Marrocchesi, Pier
Simone/N-9068-2015; Yoon, Young Soo/O-8580-2014;
OI maestro, paolo/0000-0002-4193-1288; Beatty, James/0000-0003-0481-4952;
Marrocchesi, Pier Simone/0000-0003-1966-140X; Yoon, Young
Soo/0000-0001-7023-699X; Bigongiari, Gabriele/0000-0003-3691-0826
FU NASA [NNX08AC11G, NNX08AC15G, NNX08AC16G]; Creative Research Initiatives
(RCMST) of MEST/NRF; INFN
FX The work reported in this paper was supported in the U.S. by NASA grants
NNX08AC11G, NNX08AC15G, NNX08AC16G and their predecessor grants, in
Korea by the Creative Research Initiatives (RCMST) of MEST/NRF and in
Italy by INFN. The authors acknowledge NASA/WFF for provision and
operation of flight support systems; Art Ruitberg, Suong Le, and Curtis
Dunsmore of NASA/GSFC, and Carlos Urdiales of Southwest Research
Institute for assistance with HV design and potting; CERN for provision
of excellent accelerator beams; the Fermi National Accelerator Lab Thin
Films Group for high-quality polishing and aluminization of optical
elements; and Columbia Scientific Ballooning Facility, National Science
Foundation's Office of Polar Programs, and Raytheon Polar Services
Company for outstanding support of launch, flight and recovery
operations in Antarctica.
NR 30
TC 18
Z9 18
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1400
EP 1407
DI 10.1088/0004-637X/715/2/1400
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100054
ER
PT J
AU Abbott, BP
Abbott, R
Acernese, F
Adhikari, R
Ajith, P
Allen, B
Allen, G
Alshourbagy, M
Amin, RS
Anderson, SB
Anderson, WG
Antonucci, F
Aoudia, S
Arain, MA
Araya, M
Armandula, H
Armor, P
Arun, KG
Aso, Y
Aston, S
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Baker, P
Ballardin, G
Ballmer, S
Barker, C
Barker, D
Barone, F
Barr, B
Barriga, P
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Bauer, TS
Behnke, B
Beker, M
Benacquista, M
Betzwieser, J
Beyersdorf, PT
Bigotta, S
Bilenko, IA
Billingsley, G
Birindelli, S
Biswas, R
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Boccara, C
Bodiya, TP
Bogue, L
Bondu, F
Bonelli, L
Bork, R
Boschi, V
Bose, S
Bosi, L
Braccini, S
Bradaschia, C
Brady, PR
Braginsky, VB
Brau, JE
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Brooks, AF
Brown, DA
Brummit, A
Brunet, G
Budzynski, R
Bulik, T
Bullington, A
Bulten, HJ
Buonanno, A
Burmeister, O
Buskulic, D
Byer, RL
Cadonati, L
Cagnoli, G
Calloni, E
Camp, JB
Campagna, E
Cannizzo, J
Cannon, KC
Canuel, B
Cao, J
Carbognani, F
Cardenas, L
Caride, S
Castaldi, G
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chalermsongsak, T
Chalkley, E
Charlton, P
Chassande-Mottin, E
Chatterji, S
Chelkowski, S
Chen, Y
Chincarini, A
Christensen, N
Chung, CTY
Clark, D
Clark, J
Clayton, JH
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Cokelaer, T
Colacino, CN
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Colla, A
Colombini, M
Conte, R
Cook, D
Corbitt, TRC
Corda, C
Cornish, N
Corsi, A
Coulon, JP
Coward, D
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Culter, RM
Cumming, A
Cunningham, L
Cuoco, E
Danilishin, SL
D'Antonio, S
Danzmann, K
Dari, A
Dattilo, V
Daudert, B
Davier, M
Davies, G
Daw, EJ
Day, R
De Rosa, R
DeBra, D
Degallaix, J
del Prete, M
Dergachev, V
Desai, S
DeSalvo, R
Dhurandhar, S
Di Fiore, L
Di Lieto, A
Emilio, MD
Di Virgilio, A
Diaz, M
Dietz, A
Donovan, F
Dooley, KL
Doomes, EE
Drago, M
Drever, RWP
Dueck, J
Duke, I
Dumas, JC
Dwyer, JG
Echols, C
Edgar, M
Edwards, M
Effler, A
Ehrens, P
Espinoza, E
Etzel, T
Evans, M
Evans, T
Fafone, V
Fairhurst, S
Faltas, Y
Fan, Y
Fazi, D
Fehrmann, H
Ferrante, I
Fidecaro, F
Finn, LS
Fiori, I
Flaminio, R
Flasch, K
Foley, S
Forrest, C
Fotopoulos, N
Fournier, JD
Franc, J
Franzen, A
Frasca, S
Frasconi, F
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Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, T
Fritschel, P
Frolov, VV
Fyffe, M
Galdi, V
Gammaitoni, L
Garofoli, JA
Garufi, F
Gemme, G
Genin, E
Gennai, A
Gholami, I
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Goda, K
Goetz, E
Goggin, LM
Gonzalez, G
Gorodetsky, ML
Goezetler, S
Gossler, S
Gouaty, R
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Abbott, R.
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Ajith, P.
Allen, B.
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Amin, R. S.
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Astone, P.
Aufmuth, P.
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Ballardin, G.
Ballmer, S.
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Barsuglia, M.
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Chalkley, E.
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Chen, Y.
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Christensen, N.
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Day, R.
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DeBra, D.
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del Prete, M.
Dergachev, V.
Desai, S.
DeSalvo, R.
Dhurandhar, S.
Di Fiore, L.
Di Lieto, A.
Emilio, M. Di Paolo
Di Virgilio, A.
Diaz, M.
Dietz, A.
Donovan, F.
Dooley, K. L.
Doomes, E. E.
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Drever, R. W. P.
Dueck, J.
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Dumas, J. -C.
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Edgar, M.
Edwards, M.
Effler, A.
Ehrens, P.
Espinoza, E.
Etzel, T.
Evans, M.
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Fafone, V.
Fairhurst, S.
Faltas, Y.
Fan, Y.
Fazi, D.
Fehrmann, H.
Ferrante, I.
Fidecaro, F.
Finn, L. S.
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Flaminio, R.
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Foley, S.
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Frasca, S.
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Freise, A.
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Fricke, T.
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Fyffe, M.
Galdi, V.
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Giazotto, A.
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Wilmut, I.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
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Yamamoto, H.
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CA LIGO Sci Collaboration
Virgo Collaboration
TI SEARCH FOR GRAVITATIONAL-WAVE BURSTS ASSOCIATED WITH GAMMA-RAY BURSTS
USING DATA FROM LIGO SCIENCE RUN 5 AND VIRGO SCIENCE RUN 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gravitational waves
ID 25 APRIL 1998; SHORT-DURATION GRBS; REDSHIFT DISTRIBUTIONS; LUMINOSITY
FUNCTION; RELATIVISTIC JETS; UNUSUAL SUPERNOVA; INVERSE PROBLEM; LOCAL
UNIVERSE; ACCRETION DISK; CORE-COLLAPSE
AB We present the results of a search for gravitational-wave bursts (GWBs) associated with 137 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments during the fifth LIGO science run and first Virgo science run. The data used in this analysis were collected from 2005 November 4 to 2007 October 1, and most of the GRB triggers were from the Swift satellite. The search uses a coherent network analysis method that takes into account the different locations and orientations of the interferometers at the three LIGO-Virgo sites. We find no evidence for GWB signals associated with this sample of GRBs. Using simulated short-duration (<1 s) waveforms, we set upper limits on the amplitude of gravitational waves associated with each GRB. We also place lower bounds on the distance to each GRB under the assumption of a fixed energy emission in gravitational waves, with a median limit of D similar to 12 Mpc(E-GW(iso)/0.01 M(circle dot)c(2))(1/2) for emission at frequencies around 150 Hz, where the LIGO-Virgo detector network has best sensitivity. We present astrophysical interpretations and implications of these results, and prospects for corresponding searches during future LIGO-Virgo runs.
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[Coccia, E.; Morgia, A.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
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[Dari, A.; Neri, I.] Univ Perugia, I-6123 Perugia, Italy.
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RP Abbott, BP (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA.
RI Ward, Robert/I-8032-2014; Harms, Jan/J-4359-2012; Ferrante,
Isidoro/F-1017-2012; Travasso, Flavio/J-9595-2016; Bartos,
Imre/A-2592-2017; Cella, Giancarlo/A-9946-2012; Cesarini,
Elisabetta/C-4507-2017; Frey, Raymond/E-2830-2016; Di Virgilio, Angela
Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Vecchio,
Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Khan,
Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Postiglione, Fabio/O-4744-2015; Rocchi,
Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Biswas,
Rahul/H-7474-2016; mosca, simona/I-7116-2012; Frasconi,
Franco/K-1068-2016; Sigg, Daniel/I-4308-2015; Pinto,
Innocenzo/L-3520-2016; Ju, Li/C-2623-2013; Drago, Marco/E-7134-2013; Re,
Virginia /F-6403-2013; Pitkin, Matthew/I-3802-2013; Vyatchanin,
Sergey/J-2238-2012; Khazanov, Efim/B-6643-2014; Salemi,
Francesco/F-6988-2014; Lucianetti, Antonio/G-7383-2014; Losurdo,
Giovanni/K-1241-2014; Lam, Ping Koy/A-5276-2008; Danilishin,
Stefan/K-7262-2012; Canuel, Benjamin/C-7459-2014; Khalili,
Farit/D-8113-2012; Strigin, Sergey/I-8337-2012; Cuoco,
Elena/I-8789-2012; Vicere, Andrea/J-1742-2012; Mitrofanov,
Valery/D-8501-2012; Puppo, Paola/J-4250-2012; Colla,
Alberto/J-4694-2012; Rapagnani, Piero/J-4783-2012; Gemme,
Gianluca/C-7233-2008; 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; Freise, Andreas/F-8892-2011; Marchesoni,
Fabio/A-1920-2008; Kawabe, Keita/G-9840-2011; Bondu,
Francois/A-2071-2012; Toncelli, Alessandra/A-5352-2012; Hammond,
Giles/A-8168-2012; Vocca, Helios/F-1444-2010; Finn, Lee
Samuel/A-3452-2009; Prato, Mirko/D-8531-2012; prodi,
giovanni/B-4398-2010; Santamaria, Lucia/A-7269-2012; Prokhorov,
Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Punturo,
Michele/I-3995-2012; Bigotta, Stefano/F-8652-2011; Neri,
Igor/F-1482-2010; Galdi, Vincenzo/B-1670-2008; Hammond,
Giles/B-7861-2009; Gammaitoni, Luca/B-5375-2009; McClelland,
David/E-6765-2010; Hild, Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010;
Strain, Kenneth/D-5236-2011; Acernese, Fausto/E-4989-2010; Raab,
Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck,
Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011;
OI Nishizawa, Atsushi/0000-0003-3562-0990; calloni,
enrico/0000-0003-4819-3297; Sorazu, Borja/0000-0002-6178-3198;
O'Shaughnessy, Richard/0000-0001-5832-8517; Matichard,
Fabrice/0000-0001-8982-8418; Pinto, Innocenzo M./0000-0002-2679-4457;
Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870;
Minelli, Jeff/0000-0002-5330-912X; Santamaria,
Lucia/0000-0002-5986-0449; Pierro, Vincenzo/0000-0002-6020-5521; Hallam,
Jonathan Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296;
Coccia, Eugenio/0000-0002-6669-5787; Drago, Marco/0000-0002-3738-2431;
Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447;
Whelan, John/0000-0001-5710-6576; Vedovato,
Gabriele/0000-0001-7226-1320; LONGO, Maurizio/0000-0001-8325-4003;
Fairhurst, Stephen/0000-0001-8480-1961; Boschi,
Valerio/0000-0001-8665-2293; Ferrante, Isidoro/0000-0002-0083-7228;
Travasso, Flavio/0000-0002-4653-6156; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Frey, Raymond/0000-0003-0341-2636; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414;
Stein, Leo/0000-0001-7559-9597; Milano, Leopoldo/0000-0001-9487-5876;
Vecchio, Alberto/0000-0002-6254-1617; Khan, Rubab/0000-0001-5100-5168;
Garufi, Fabio/0000-0003-1391-6168; Postiglione,
Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Biswas,
Rahul/0000-0002-0774-8906; mosca, simona/0000-0001-7869-8275; Frasconi,
Franco/0000-0003-4204-6587; Sigg, Daniel/0000-0003-4606-6526; Pitkin,
Matthew/0000-0003-4548-526X; Losurdo, Giovanni/0000-0003-0452-746X; Lam,
Ping Koy/0000-0002-4421-601X; Danilishin, Stefan/0000-0001-7758-7493;
Vicere, Andrea/0000-0003-0624-6231; Puppo, Paola/0000-0003-4677-5015;
Gemme, Gianluca/0000-0002-1127-7406; Allen, Bruce/0000-0003-4285-6256;
Zhao, Chunnong/0000-0001-5825-2401; Marchesoni,
Fabio/0000-0001-9240-6793; Bondu, Francois/0000-0001-6487-5197;
Toncelli, Alessandra/0000-0003-4400-8808; Vocca,
Helios/0000-0002-1200-3917; Finn, Lee Samuel/0000-0002-3937-0688; Prato,
Mirko/0000-0002-2188-8059; prodi, giovanni/0000-0001-5256-915X;
Gorodetsky, Michael/0000-0002-5159-2742; Punturo,
Michele/0000-0001-8722-4485; Neri, Igor/0000-0002-9047-9822; Galdi,
Vincenzo/0000-0002-4796-3600; Gammaitoni, Luca/0000-0002-4972-7062;
McClelland, David/0000-0001-6210-5842; Strain,
Kenneth/0000-0002-2066-5355; Acernese, Fausto/0000-0003-3103-3473;
Lueck, Harald/0000-0001-9350-4846; Whiting, Bernard
F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Principe,
Maria/0000-0002-6327-0628; Papa, M.Alessandra/0000-0002-1007-5298;
Kanner, Jonah/0000-0001-8115-0577; Granata, Massimo/0000-0003-3275-1186;
Aulbert, Carsten/0000-0002-1481-8319; Di Paolo Emilio,
Maurizio/0000-0002-9558-3610; PERSICHETTI, GIANLUCA/0000-0001-8424-9791;
Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946
FU 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; Netherlands
Organisation for Scientific Research; Royal Society; Scottish Funding
Council; Scottish Universities Physics Alliance; National Aeronautics
and Space Administration; Carnegie Trust; Leverhulme Trust; David and
Lucile Packard Foundation; Research Corporation; Alfred P. Sloan
Foundation
FX We are indebted to the observers of the electromagnetic events and the
GCN for providing us with valuable data. The authors gratefully
acknowledge the support of the United States National Science Foundation
for the construction and operation of the LIGO Laboratory, the Science
and Technology Facilities Council of the United Kingdom, the
Max-Planck-Society, and the State of Niedersachsen/Germany for support
of the construction and operation of the GEO600 detector, and the
Italian Istituto Nazionale di Fisica Nucleare and the French Centre
National de la Recherche Scientifique for the construction and operation
of the Virgo detector. The authors also gratefully acknowledge research
support 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 Foundation for Fundamental Research
on Matter supported by the Netherlands Organisation for Scientific
Research, 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. This document has been assigned LIGO Laboratory
document number LIGO-P0900023-v16.
NR 97
TC 52
Z9 52
U1 3
U2 41
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1438
EP 1452
DI 10.1088/0004-637X/715/2/1438
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100057
ER
PT J
AU Abadie, J
Abbott, BP
Abbott, R
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O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Pagliaroli, G
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Papa, MA
Pardi, S
Parisi, M
Pasqualetti, A
Passaquieti, R
Passuello, D
Patel, P
Pathak, D
Pedraza, M
Pekowsky, L
Penn, S
Peralta, C
Perreca, A
Persichetti, G
Pichot, M
Pickenpack, M
Piergiovanni, F
Pietka, M
Pinard, L
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Poggiani, R
Postiglione, F
Prato, M
Predoi, V
Principe, M
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Raab, FJ
Rabeling, DS
Radkins, H
Raffai, P
Raics, Z
Rakhmanov, M
Rapagnani, P
Raymond, V
Re, V
Reed, CM
Reed, T
Regimbau, T
Rehbein, H
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Roberts, P
Robertson, NA
Robinet, F
Robinson, C
Robinson, EL
Rocchi, A
Roddy, S
Rover, C
Rolland, L
Rollins, J
Romano, JD
Romano, R
Romie, JH
Rosinska, D
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Sakata, S
Salemi, F
Sammut, L
de la Jordana, LS
Sandberg, V
Sannibale, V
Santamaria, L
Santostasi, G
Saraf, S
Sarin, P
Sassolas, B
Sathyaprakash, BS
Sato, S
Satterthwaite, M
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, R
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Searle, AC
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sergeev, A
Shapiro, B
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Sintes, AM
Skelton, G
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, ND
Somiya, K
Sorazu, B
Stein, AJ
Stein, LC
Steplewski, S
Stochino, A
Stone, R
Strain, KA
Strigin, S
Stroeer, A
Sturani, R
Stuver, AL
Summerscales, TZ
Sung, M
Susmithan, S
Sutton, PJ
Swinkels, B
Szokoly, GP
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, JR
Taylor, R
Thorne, KA
Thorne, KS
Thuring, A
Titsler, C
Tokmakov, KV
Toncelli, A
Tonelli, M
Torres, C
Torrie, CI
Tournefier, E
Travasso, F
Traylor, G
Trias, M
Trummer, J
Turner, L
Ugolini, D
Urbanek, K
Vahlbruch, H
Vajente, G
Vallisneri, M
van den Brand, JFJ
Van Den Broeck, C
van der Putten, S
van der Sluys, MV
Vass, S
Vaulin, R
Vavoulidis, M
Vecchio, A
Vedovato, G
van Veggel, AA
Veitch, J
Veitch, PJ
Veltkamp, C
Verkindt, D
Vetrano, F
Vicere, A
Villar, A
Vinet, JY
Vocca, H
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Wanner, A
Ward, RL
Was, M
Wei, P
Weinert, M
Weinstein, AJ
Weiss, R
Wen, L
Wen, S
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Wilmut, I
Winkelmann, L
Winkler, W
Wipf, CC
Wiseman, AG
Woan, G
Wooley, R
Worden, J
Yakushin, I
Yamamoto, H
Yamamoto, K
Yeaton-Massey, D
Yoshida, S
Yu, PP
Yvert, M
Zanolin, M
Zhang, L
Zhang, Z
Zhao, C
Zotov, N
Zucker, ME
Zweizig, J
AF Abadie, J.
Abbott, B. P.
Abbott, R.
Accadia, T.
Acernese, F.
Adhikari, R.
Ajith, P.
Allen, B.
Allen, G.
Ceron, E. Amador
Amin, R. S.
Anderson, S. B.
Anderson, W. G.
Antonucci, F.
Aoudia, S.
Arain, M. A.
Araya, M.
Arun, K. G.
Aso, Y.
Aston, S.
Astone, P.
Aufmuth, P.
Aulbert, C.
Babak, S.
Baker, P.
Ballardin, G.
Ballmer, S.
Barker, D.
Barone, F.
Barr, B.
Barriga, P.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Bastarrika, M.
Bauer, Th. S.
Behnke, B.
Beker, M. G.
Belletoile, A.
Benacquista, M.
Betzwieser, J.
Beyersdorf, P. T.
Bigotta, S.
Bilenko, I. A.
Billingsley, G.
Birindelli, S.
Biswas, R.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Bland, B.
Blom, M.
Boccara, C.
Bock, O.
Bodiya, T. P.
Bondarescu, R.
Bondu, F.
Bonelli, L.
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Born, M.
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Overmier, H.
Owen, B. J.
Page, A.
Pagliaroli, G.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Papa, M. A.
Pardi, S.
Parisi, M.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Patel, P.
Pathak, D.
Pedraza, M.
Pekowsky, L.
Penn, S.
Peralta, C.
Perreca, A.
Persichetti, G.
Pichot, M.
Pickenpack, M.
Piergiovanni, F.
Pietka, M.
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Pitkin, M.
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Rabeling, D. S.
Radkins, H.
Raffai, P.
Raics, Z.
Rakhmanov, M.
Rapagnani, P.
Raymond, V.
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Reed, C. M.
Reed, T.
Regimbau, T.
Rehbein, H.
Reid, S.
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Riesen, R.
Riles, K.
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Robinson, C.
Robinson, E. L.
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Sammut, L.
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Sandberg, V.
Sannibale, V.
Santamaria, L.
Santostasi, G.
Saraf, S.
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Sassolas, B.
Sathyaprakash, B. S.
Sato, S.
Satterthwaite, M.
Saulson, P. R.
Savage, R.
Schilling, R.
Schnabel, R.
Schofield, R.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Searle, A. C.
Seifert, F.
Sellers, D.
Sengupta, A. S.
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Sergeev, A.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
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Sintes, A. M.
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Ward, R. L.
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Weinert, M.
Weinstein, A. J.
Weiss, R.
Wen, L.
Wen, S.
Wessels, P.
West, M.
Westphal, T.
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.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Yakushin, I.
Yamamoto, H.
Yamamoto, K.
Yeaton-Massey, D.
Yoshida, S.
Yu, P. P.
Yvert, M.
Zanolin, M.
Zhang, L.
Zhang, Z.
Zhao, C.
Zotov, N.
Zucker, M. E.
Zweizig, J.
CA LIGO Sci Collaboration
VIRGO Collaboration
TI SEARCH FOR GRAVITATIONAL-WAVE INSPIRAL SIGNALS ASSOCIATED WITH SHORT
GAMMA-RAY BURSTS DURING LIGO'S FIFTH AND VIRGO'S FIRST SCIENCE RUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; gamma-ray burst: general; gravitational waves
ID NEUTRON-STAR MERGERS; COMPACT BINARIES; MISSION; SUPERNOVA;
INTERFEROMETER; SGR-1806-20; GRB-060614; GRB-070201; ORIGIN; FLARE
AB Progenitor scenarios for short gamma-ray bursts (short GRBs) include coalescenses of two neutron stars or a neutron star and black hole, which would necessarily be accompanied by the emission of strong gravitational waves. We present a search for these known gravitational-wave signatures in temporal and directional coincidence with 22 GRBs that had sufficient gravitational-wave data available in multiple instruments during LIGO's fifth science run, S5, and Virgo's first science run, VSR1. We find no statistically significant gravitational-wave candidates within a [-5, +1) s window around the trigger time of any GRB. Using the Wilcoxon-Mann-Whitney U-test, we find no evidence for an excess of weak gravitational-wave signals in our sample of GRBs. We exclude neutron star-black hole progenitors to a median 90% confidence exclusion distance of 6.7 Mpc.
C1 [Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Anderson, S. B.; Araya, M.; Aso, Y.; Ballmer, S.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chatterji, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Driggers, J.; Ehrens, P.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Mak, C.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Mitra, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Sannibale, V.; Searle, A. C.; Seifert, F.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Turner, L.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] LIGO CALTECH, Pasadena, CA 91125 USA.
[Accadia, T.; Belletoile, A.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Trummer, J.; Verkindt, D.; Yvert, M.] Univ Savoie, LAPP, CNRS, IN2P3, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; De Rosa, R.; Di Fiore, L.; Garufi, F.; Milano, L.; Mosca, S.; Pardi, S.; Parisi, M.; Persichetti, G.; Romano, R.] Complesso Univ Monte St Angelo, Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Acernese, F.; Barone, F.; Conte, R.; Postiglione, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Allen, B.; Aulbert, C.; Bock, O.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmann, H.; Frede, M.; Friedrich, D.; Giampanis, S.; Gossler, S.; Grote, H.; Hayama, K.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kullman, J.; Lastzka, N.; Leaci, P.; Lueck, H.; Machenschalk, B.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Prix, R.; Puncken, O.; Rehbein, H.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Willke, B.; Winkelmann, L.; Winkler, W.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Biswas, R.; Brady, P. R.; Burguet-Castell, J.; Clayton, J. H.; Creighton, J. D. E.; Flasch, K.; Fotopoulos, N.; Goggin, L. M.; Hammer, D.; Koranda, S.; Mercer, R. A.; Moe, B.; Oldenburg, R.; Papa, M. A.; Siemens, X.; Skelton, G.; Vaulin, R.; Wiseman, A. G.; Yu, P. P.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, G.; Bullington, A.; Byer, R. L.; Clark, D.; DeBra, D.; Lantz, B.; Leindecker, N.; Lu, P.; Markosyan, A.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA.
[Amin, R. S.; Caudill, S.; Fricke, T. T.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kissel, J. S.; Matichard, F.; Slutsky, J.; Sung, M.; Wen, S.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Antonucci, F.; Astone, P.; Colla, A.; Corsi, A.; Frasca, S.; Majorana, E.; Moscatelli, V.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] INFN, Sez Roma, I-00185 Rome, Italy.
[Aoudia, S.; Birindelli, S.; Brillet, A.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Greverie, C.; Heitmann, H.; Man, N.; Pichot, M.; Regimbau, T.; Vinet, J. -Y.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Arain, M. A.; Dooley, K. L.; Faltas, Y.; Klimenko, S.; Lin, H.; Lucianetti, A.; Martin, R. M.; Mitselmakher, G.; Mueller, G.; Ottens, R. S.; Pankow, C.; Quetschke, V.; Reitze, D. H.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Arun, K. G.; Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Hello, P.; Leroy, N.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, LAL, CNRS, IN2P3, F-91898 Orsay, France.
[Aston, S.; Chelkowski, S.; Cruise, A. M.; Culter, R. M.; Freise, A.; Fulda, P.; Hallam, J. M.; Hoyland, D.; Lodhia, D.; Page, A.; Perreca, A.; Vecchio, A.; Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Aufmuth, P.; Danzmann, K.; Hage, B.; Kwee, P.; Lueck, H.; Thuering, A.; Vahlbruch, H.; Willke, B.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Papa, M. A.; Peralta, C.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P.; Cornish, N.; Littenberg, T. B.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Colas, J.; Cuoco, E.; Dattilo, V.; Day, R.; Fiori, I.; Genin, E.; Huet, D.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.] EGO, I-56021 Cascina, Pi, Italy.
[Barker, D.; Barton, M. A.; Bland, B.; Cook, D.; Effler, A.; Gray, C.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Ryan, K.; Sandberg, V.; Savage, R.; Schwinberg, P.; Sigg, D.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Barr, B.; Bassiri, R.; Bastarrika, M.; Chalkley, E.; Cumming, A.; Cunningham, L.; Edgar, M.; Grant, A.; Hammond, G. D.; Haughian, K.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Martin, I. W.; Miller, J.; Murray, P. G.; Nawrodt, R.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Scott, J.; Sorazu, B.; Strain, K. A.; Tokmakov, K. V.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland.
[Barriga, P.; Blair, D.; Coward, D.; Dumas, J. -C.; Fan, Y.; Gras, S.; Howell, E.; Ju, L.; Merill, L.; Miao, H.; Susmithan, S.; Wen, L.; Zhang, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Barsotti, L.; Blackburn, L.; Bodiya, T. P.; Cao, J.; Corbitt, T. R. C.; Donovan, F.; Duke, I.; Evans, M.; Foley, S.; Fritschel, P.; Harry, G. M.; Hughey, B.; Katsavounidis, E.; MacInnis, M.; Markowitz, J.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Sarin, P.; Shapiro, B.; Shoemaker, D. H.; Smith, N. D.; Stein, A. J.; Stein, L. C.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] LIGO MIT, Cambridge, MA 02139 USA.
[Barsuglia, M.; Buy, C.; Chassande-Mottin, E.; Granata, M.] Univ Denis Diderot Paris 7, CNRS, IN2P3, Observ Paris,DSM,IRFU,CEA,UMR7164, Paris, France.
[Bartos, I.; Khan, R.; Marka, S.; Marka, Z.; Matone, L.; Raics, Z.; Rollins, J.] Columbia Univ, New York, NY 10027 USA.
[Bauer, Th. S.; Blom, M.; Bulten, H. J.; Li, T. G. F.; Rabeling, D. S.; van den Brand, J. F. J.; van der Putten, S.] Nikhef, Natl Inst Subatom Phys, NL-1009 DB Amsterdam, Netherlands.
[Beker, M. G.; Benacquista, M.; Creighton, T. D.; Diaz, M.; Grosso, R.; Mohanty, S. D.; Mukherjee, S.; Rakhmanov, M.; Romano, J. D.; Stone, R.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA.
[Beyersdorf, P. T.] San Jose State Univ, San Jose, CA 95192 USA.
[Bigotta, S.; Bonelli, L.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; del Prete, M.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Paoletti, F.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] INFN, Sez Pisa, I-56127 Pisa, Italy.
[Bigotta, S.; Bonelli, L.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56127 Pisa, Italy.
[Bilenko, I. A.; Braginsky, V. B.; Danilishin, S. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Tarabrin, S. P.; Vyachanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Boccara, C.; Loriette, V.; Maksimovic, I.; Moreau, J.] CNRS, ESPCI, F-75005 Paris, France.
[Bondarescu, R.; Finn, L. S.; Kopparapu, R.; Lang, M.; Menendez, D. F.; O'Shaughnessy, R.; Owen, B. J.; Titsler, C.; Williams, H. R.] Penn State Univ, University Pk, PA 16802 USA.
[Bondu, F.] Univ Rennes 1, Inst Phys Rennes, CNRS, F-35042 Rennes, France.
[Bonnand, R.; Flaminio, R.; Franc, J.; Galimberti, M.; Michel, C.; Morgado, N.; Pinard, L.; Sassolas, B.] CNRS, LMA, IN2P3, F-69622 Lyon, France.
[Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Bosi, L.; Gammaitoni, L.; Marchesoni, F.; Neri, I.; Punturo, M.; Travasso, F.; Vocca, H.] INFN, Sez Perugia, I-6123 Perugia, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Schofield, R.] Univ Oregon, Eugene, OR 97403 USA.
[Bridges, D. O.; Evans, T.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Hanson, J.; Hoak, D.; Holt, K.; Lormand, M.; Meyer, M. S.; O'Reilly, B.; Overmier, H.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Sibley, A.; Stuver, A. L.; Thorne, K. A.; Torres, C.; Traylor, G.; Wooley, R.; Yakushin, I.] Livingston Observ, LIGO, Livingston, LA 70754 USA.
[Brown, D. A.; Capano, C. D.; Garofoli, J. A.; Hirose, E.; Lundgren, A.; Pekowsky, L.; Saulson, P. R.; Smith, J. R.; Wei, P.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Budzynski, R.] Warsaw Univ, PL-00681 Warsaw, Poland.
[Bulik, T.; Kowalska, I.] Warsaw Univ, Astro Obs, PL-00478 Warsaw, Poland.
[Bulik, T.] CAMK PAN, PL-00716 Warsaw, Poland.
[Bulten, H. J.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Buonanno, A.; Kanner, J.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA.
[Cagnoli, G.; Campagna, E.; Guidi, G. M.; Lorenzini, M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy.
[Cain, J.; Cavaglia, M.] Univ Mississippi, University, MS 38677 USA.
[Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.; Mosca, S.; Pardi, S.; Parisi, M.; Persichetti, G.] Univ Naples Federico II, I-80126 Naples, Italy.
[Camp, J. B.; Cannizzo, J.; Stroeer, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Campagna, E.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Chen, Y.; Mino, Y.; Somiya, K.; Thorne, K. S.; Vallisneri, M.; Wen, L.] CALTECH, CaRT, Pasadena, CA 91125 USA.
[Chincarini, A.; Gemme, G.; Prato, M.] INFN, Sez Genova, I-16146 Genoa, Italy.
[Christensen, N.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA.
[Chua, S. S. Y.; Lam, P. K.; McClelland, D. E.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Satterthwaite, M.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Clark, J.; Davies, G.; Edwards, M.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Minenkov, Y.; Pathak, D.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Coccia, E.; D'Antonio, S.; Emilio, M. Di Paolo; Fafone, V.; Morgia, A.; Pagliaroli, G.; Rocchi, A.] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Coccia, E.; Fafone, V.; Morgia, A.; Pagliaroli, G.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Colla, A.; Colombini, M.; Frasca, S.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Daw, E. J.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[del Prete, M.; Mantovani, M.] Univ Siena, I-53100 Siena, Italy.
[Dergachev, V.; Goetz, E.; Gustafson, R.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Dhurandhar, S.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Emilio, M. Di Paolo] Univ Aquila, I-67100 Laquila, Italy.
[Doomes, E. E.; McGuire, S. C.] INAF, IFSI, I-00133 Rome, Italy.
[Drago, M.; Vedovato, G.] INFN, Sez Padova, I-35131 Padua, Italy.
[Drago, M.] Univ Padua, I-35131 Padua, Italy.
[Forrest, C.; Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Frei, M.; Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[Frei, Z.; Raffai, P.; Szokoly, G. P.] Eutvus Univ, ELTE, H-1053 Budapest, Hungary.
[Gammaitoni, L.; Neri, I.; Travasso, F.] Univ Perugia, I-6123 Perugia, Italy.
[Greenhalgh, R. J. S.; Hayler, T.; O'Dell, J.; Wilmut, I.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Gretarsson, A. M.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Harms, J.; Kandhasamy, S.; Mandic, V.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Husa, S.; Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain.
[Jaranowski, P.; Pietka, M.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Kalogera, V.; Mandel, I.; Raymond, V.; van der Sluys, M. V.] Northwestern Univ, Evanston, IL 60208 USA.
[Kawamura, S.; Kokeyama, K.; Nishida, E.; Nishizawa, A.; Sakata, S.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Khazanov, E.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Krolak, A.] IPJ, PL-05400 Otwock, Poland.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Prodi, G. A.; Re, V.] Grp Collegato Trento, INFN, I-38050 Trento, Italy.
[Prodi, G. A.; Re, V.] Univ Trent, I-38050 Trento, Italy.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Roberts, P.; Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA.
[Saraf, S.] Sonoma State Univ, Rohnert Pk, CA 94928 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
[Drever, R. W. P.] CALTECH, Pasadena, CA 91125 USA.
RP Abadie, J (reprint author), LIGO CALTECH, Pasadena, CA 91125 USA.
RI Ward, Robert/I-8032-2014; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Ferrante, Isidoro/F-1017-2012; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Cella,
Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Frey,
Raymond/E-2830-2016; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Mow-Lowry, Conor/F-8843-2015; Khan,
Rubab/F-9455-2015; Finn, Lee Samuel/A-3452-2009; Ottaway,
David/J-5908-2015; Garufi, Fabio/K-3263-2015; Postiglione,
Fabio/O-4744-2015; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Howell, Eric/H-5072-2014; Biswas,
Rahul/H-7474-2016; mosca, simona/I-7116-2012; Frasconi,
Franco/K-1068-2016; Sigg, Daniel/I-4308-2015; Pitkin,
Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Miao,
Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Salemi,
Francesco/F-6988-2014; Lucianetti, Antonio/G-7383-2014; Nawrodt,
Ronny/J-5155-2014; Losurdo, Giovanni/K-1241-2014; Lam, Ping
Koy/A-5276-2008; Danilishin, Stefan/K-7262-2012; Canuel,
Benjamin/C-7459-2014; Khalili, Farit/D-8113-2012; Vecchio,
Alberto/F-8310-2015; Mitrofanov, Valery/D-8501-2012; Puppo,
Paola/J-4250-2012; Colla, Alberto/J-4694-2012; Rapagnani,
Piero/J-4783-2012; Gemme, Gianluca/C-7233-2008; 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; Parisi, Maria/D-2817-2013; Drago, Marco/E-7134-2013; Re,
Virginia /F-6403-2013; Marchesoni, Fabio/A-1920-2008; Kawabe,
Keita/G-9840-2011; Bondu, Francois/A-2071-2012; Toncelli,
Alessandra/A-5352-2012; Hammond, Giles/A-8168-2012; Vocca,
Helios/F-1444-2010; Prato, Mirko/D-8531-2012; prodi,
giovanni/B-4398-2010; Santamaria, Lucia/A-7269-2012; Prokhorov,
Leonid/I-2953-2012; Punturo, Michele/I-3995-2012; Strigin,
Sergey/I-8337-2012; Cuoco, Elena/I-8789-2012; Vicere,
Andrea/J-1742-2012; McClelland, David/E-6765-2010; Hild,
Stefan/A-3864-2010; Rowan, Sheila/E-3032-2010; Strain,
Kenneth/D-5236-2011; Acernese, Fausto/E-4989-2010; Raab,
Frederick/E-2222-2011; Martin, Iain/A-2445-2010; Lueck,
Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Bigotta,
Stefano/F-8652-2011; Neri, Igor/F-1482-2010; Hammond, Giles/B-7861-2009;
Gammaitoni, Luca/B-5375-2009; Freise, Andreas/F-8892-2011;
OI Pathak, Devanka/0000-0002-1768-8353; Granata,
Massimo/0000-0003-3275-1186; Aulbert, Carsten/0000-0002-1481-8319; Di
Paolo Emilio, Maurizio/0000-0002-9558-3610; PERSICHETTI,
GIANLUCA/0000-0001-8424-9791; Freise, Andreas/0000-0001-6586-9901;
Mandel, Ilya/0000-0002-6134-8946; calloni, enrico/0000-0003-4819-3297;
Sorazu, Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397;
O'Shaughnessy, Richard/0000-0001-5832-8517; Husa,
Sascha/0000-0002-0445-1971; Pinto, Innocenzo M./0000-0002-2679-4457;
Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870;
Santamaria, Lucia/0000-0002-5986-0449; Coccia,
Eugenio/0000-0002-6669-5787; Hallam, Jonathan Mark/0000-0002-7087-0461;
Vetrano, Flavio/0000-0002-7523-4296; Nishizawa,
Atsushi/0000-0003-3562-0990; Drago, Marco/0000-0002-3738-2431; Ward,
Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan,
John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320;
Fairhurst, Stephen/0000-0001-8480-1961; Matichard,
Fabrice/0000-0001-8982-8418; Ferrante, Isidoro/0000-0002-0083-7228;
Travasso, Flavio/0000-0002-4653-6156; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Frey, Raymond/0000-0003-0341-2636; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414;
Stein, Leo/0000-0001-7559-9597; Milano, Leopoldo/0000-0001-9487-5876;
Khan, Rubab/0000-0001-5100-5168; Finn, Lee Samuel/0000-0002-3937-0688;
Garufi, Fabio/0000-0003-1391-6168; Postiglione,
Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Howell, Eric/0000-0001-7891-2817;
Biswas, Rahul/0000-0002-0774-8906; mosca, simona/0000-0001-7869-8275;
Frasconi, Franco/0000-0003-4204-6587; Sigg, Daniel/0000-0003-4606-6526;
Pitkin, Matthew/0000-0003-4548-526X; Miao, Haixing/0000-0003-4101-9958;
Losurdo, Giovanni/0000-0003-0452-746X; Lam, Ping
Koy/0000-0002-4421-601X; Danilishin, Stefan/0000-0001-7758-7493;
Vecchio, Alberto/0000-0002-6254-1617; Puppo, Paola/0000-0003-4677-5015;
Gemme, Gianluca/0000-0002-1127-7406; Allen, Bruce/0000-0003-4285-6256;
Zhao, Chunnong/0000-0001-5825-2401; Marchesoni,
Fabio/0000-0001-9240-6793; Bondu, Francois/0000-0001-6487-5197;
Toncelli, Alessandra/0000-0003-4400-8808; Vocca,
Helios/0000-0002-1200-3917; Prato, Mirko/0000-0002-2188-8059; prodi,
giovanni/0000-0001-5256-915X; Punturo, Michele/0000-0001-8722-4485;
Vicere, Andrea/0000-0003-0624-6231; McClelland,
David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355;
Acernese, Fausto/0000-0003-3103-3473; Lueck, Harald/0000-0001-9350-4846;
Neri, Igor/0000-0002-9047-9822; Gammaitoni, Luca/0000-0002-4972-7062;
Whiting, Bernard F/0000-0002-8501-8669; Veitch,
John/0000-0002-6508-0713; Principe, Maria/0000-0002-6327-0628; Papa,
M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577
FU 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; Netherlands
Organisation for Scientific Research; Royal Society; Scottish Funding
Council; Scottish Universities Physics Alliance; National Aeronautics
and Space Administration; Carnegie Trust; Leverhulme Trust; David and
Lucile Packard Foundation; Research Corporation; Alfred P. Sloan
Foundation
FX We are indebted to the observers of the electromagnetic events and the
GCN for providing us with valuable data. The authors gratefully
acknowledge the support of the United States National Science Foundation
for the construction and operation of the LIGO Laboratory, the Science
and Technology Facilities Council of the United Kingdom, the
Max-Planck-Society, and the State of Niedersachsen/Germany for support
of the construction and operation of the GEO600 detector, and the
Italian Istituto Nazionale di Fisica Nucleare and the French Centre
National de la Recherche Scientifique for the construction and operation
of the Virgo detector. The authors also gratefully acknowledge research
support 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 Foundation for Fundamental Research
on Matter supported by the Netherlands Organisation for Scientific
Research, 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 59
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1453
EP 1461
DI 10.1088/0004-637X/715/2/1453
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100058
ER
PT J
AU Crepp, J
Serabyn, E
Carson, J
Ge, J
Kravchenko, I
AF Crepp, J.
Serabyn, E.
Carson, J.
Ge, J.
Kravchenko, I.
TI ON-SKY DEMONSTRATION OF A LINEAR BAND-LIMITED MASK WITH APPLICATION TO
VISUAL BINARY STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; instrumentation: adaptive optics; instrumentation:
high angular resolution; planetary systems
ID EPSILON-ERIDANI; PLANET FORMATION; GIANT PLANETS; CIRCUMBINARY PLANETS;
EXTRASOLAR PLANETS; ORBITAL ELEMENTS; MULTIPLE SYSTEMS; IMAGE MASKS; DQ
TAU; CORONAGRAPH
AB We have designed and built the first band-limited coronagraphic mask used for ground-based high-contrast imaging observations. The mask resides in the focal plane of the near-infrared camera PHARO at the Palomar Hale telescope and receives a well-corrected beam from an extreme adaptive optics system. Its performance on-sky with single stars is comparable to current state-of-the-art instruments: contrast levels of similar to 10(-5) or better at 0 ''.8 in K-s after post-processing, depending on how well non-common-path errors are calibrated. However, given the mask's linear geometry, we are able to conduct additional unique science observations. Since the mask does not suffer from pointing errors down its long axis, it can suppress the light from two different stars simultaneously, such as the individual components of a spatially resolved binary star system, and search for faint tertiary companions. In this paper, we present the design of the mask, the science motivation for targeting binary stars, and our preliminary results, including the detection of a candidate M-dwarf tertiary companion orbiting the visual binary star HIP 48337, which we are continuing to monitor with astrometry to determine its association.
C1 [Crepp, J.; Ge, J.; Kravchenko, I.] Univ Florida, Gainesville, FL 32611 USA.
[Crepp, J.] CALTECH, Pasadena, CA 91125 USA.
[Serabyn, E.; Carson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Carson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, J.] Coll Charleston, Charleston, SC 29424 USA.
[Kravchenko, I.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA.
RP Crepp, J (reprint author), Univ Florida, 211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
EM jcrepp@astro.caltech.edu
RI Kravchenko, Ivan/K-3022-2015
OI Kravchenko, Ivan/0000-0003-4999-5822
FU NASA [NNG06GC49G]; UCF-UF-SRI program
FX We thank Karl Stapelfeldt for support at the JPL microdevices lab to cut
and clean the BLM prior to installation, and Dimitri Mawet for helpful
conversations at the observatory. J.C. acknowledges support from the
NASA postdoctoral program. This work was funded by the UCF-UF-SRI
program and NASA grant NNG06GC49G. Part of this research was conducted
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with NASA.
NR 71
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1533
EP 1538
DI 10.1088/0004-637X/715/2/1533
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100064
ER
PT J
AU Rachmeler, LA
Pariat, E
DeForest, CE
Antiochos, S
Torok, T
AF Rachmeler, L. A.
Pariat, E.
DeForest, C. E.
Antiochos, S.
Toeroek, T.
TI SYMMETRIC CORONAL JETS: A RECONNECTION-CONTROLLED STUDY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: activity; Sun: corona
ID X-RAY JETS; COLLISIONLESS MAGNETIC RECONNECTION; TWISTED FLUX TUBES;
KINK INSTABILITY; NUMERICAL SIMULATIONS; SOLAR ATMOSPHERE; FIELD
PROPERTIES; MASS EJECTIONS; CURRENT SHEETS; ACTIVE-REGION
AB Current models and observations imply that reconnection is a key mechanism for destabilization and initiation of coronal jets. We evolve a system described by the theoretical symmetric jet formation model using two different numerical codes with the goal of studying the role of reconnection in this system. One of the codes is the Eulerian adaptive mesh code ARMS, which simulates magnetic reconnection through numerical diffusion. The quasi-Lagrangian FLUX code, on the other hand, is ideal and able to evolve the system without reconnection. The ideal nature of FLUX allows us to provide a control case of evolution without reconnection. We find that during the initial symmetric and ideal phase of evolution, both codes produce very similar morphologies and energy growth. The symmetry is then broken by a kink-like motion of the axis of rotation, after which the two systems diverge. In ARMS, current sheets formed and reconnection rapidly released the stored magnetic energy. In FLUX, the closed field remained approximately constant in height while expanding in width and did not release any magnetic energy. We find that the symmetry threshold is an ideal property of the system, but the lack of energy release implies that the observed kink is not an instability. Because of the confined nature of the FLUX system, we conclude that reconnection is indeed necessary for jet formation in symmetric jet models in a uniform coronal background field.
C1 [Rachmeler, L. A.] Univ Colorado, Boulder, CO 80304 USA.
[Pariat, E.; Toeroek, T.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France.
[DeForest, C. E.] SW Res Inst, Boulder, CO 80302 USA.
[Antiochos, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rachmeler, LA (reprint author), Univ Colorado, Boulder, CO 80304 USA.
EM laurel.rachmeler@colorado.edu
RI Antiochos, Spiro/D-4668-2012
OI Antiochos, Spiro/0000-0003-0176-4312
FU NASA; European Commission [MTRM-CT-2006-035484, 218816]
FX The authors thank P. Demoulin for insightful comments and discussions.
This work was supported in part by the NASA HTP, LWS-TR&T, and SHP-SR&T
programs. Financial support by the European Commission through the
SOLAIRE network (MTRM-CT-2006-035484) is gratefully acknowledged. The
research leading to these results has received funding from the European
Commission's Seventh Framework Program (FP7/2007-2013) under the grant
agreement 218816 (SOTERIA project, www.soteria-space.eu). The ARMS
numerical simulations were performed on DoD High Performance Computing
Modernization Program resources at NRL-DC. FLUX is open source software
available from http://flux.boulder.swri.edu. Thanks is also given to the
PDL development team http://pdl.perl.org.
NR 67
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1556
EP 1565
DI 10.1088/0004-637X/715/2/1556
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100066
ER
PT J
AU Sajina, A
Yan, L
Armus, L
Choi, P
Fadda, D
Helou, G
Spoon, H
AF Sajina, Anna
Yan, Lin
Armus, Lee
Choi, Philip
Fadda, Dario
Helou, George
Spoon, Henrik
TI SPITZER MID-INFRARED SPECTROSCOPY OF INFRARED LUMINOUS GALAXIES AT z
similar to 2. II. DIAGNOSTICS (vol 664, pg 713, 2007)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
ID ACTIVE GALACTIC NUCLEI
C1 [Sajina, Anna; Yan, Lin; Armus, Lee; Helou, George] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Choi, Philip] Pomona Coll, Claremont, CA 91711 USA.
[Fadda, Dario] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Spoon, Henrik] Cornell Univ, Ithaca, NY 14853 USA.
RP Sajina, A (reprint author), Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
NR 5
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2010
VL 715
IS 2
BP 1592
EP 1592
DI 10.1088/0004-637X/715/2/1592
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 595VR
UT WOS:000277642100070
ER
PT J
AU Hammel, HB
Wong, MH
Clarke, JT
de Pater, I
Fletcher, LN
Hueso, R
Noll, K
Orton, GS
Perez-Hoyos, S
Sanchez-Lavega, A
Simon-Miller, AA
Yanamandra-Fisher, PA
AF Hammel, H. B.
Wong, M. H.
Clarke, J. T.
de Pater, I.
Fletcher, L. N.
Hueso, R.
Noll, K.
Orton, G. S.
Perez-Hoyos, S.
Sanchez-Lavega, A.
Simon-Miller, A. A.
Yanamandra-Fisher, P. A.
TI JUPITER AFTER THE 2009 IMPACT: HUBBLE SPACE TELESCOPE IMAGING OF THE
IMPACT-GENERATED DEBRIS AND ITS TEMPORAL EVOLUTION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: general;
planets and satellites: individual (Jupiter)
ID COMET SHOEMAKER-LEVY-9; ZONAL WINDS; STRATOSPHERE; STABILITY; SPECTRUM;
AEROSOL
AB We report Hubble Space Telescope images of Jupiter during the aftermath of an impact by an unknown object in 2009 July. The 2009 impact-created debris field evolved more slowly than those created in 1994 by the collision of the tidally disrupted comet D/Shoemaker-Levy 9 (SL9). The slower evolution, in conjunction with the isolated nature of this single impact, permits a more detailed assessment of the altitudes and meridional motion of the debris than was possible with SL9. The color of the 2009 debris was markedly similar to that seen in 1994, thus this dark debris is likely to be Jovian material that is highly thermally processed. The 2009 impact site differed from the 1994 SL9 sites in UV morphology and contrast lifetime; both are suggestive of the impacting body being asteroidal rather than cometary. Transport of the 2009 Jovian debris as imaged by Hubble shared similarities with transport of volcanic aerosols in Earth's atmosphere after major eruptions.
C1 [Hammel, H. B.] Space Sci Inst, Boulder, CO 80301 USA.
[Wong, M. H.; Noll, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Wong, M. H.; de Pater, I.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Clarke, J. T.] Boston Univ, Boston, MA 02215 USA.
[Fletcher, L. N.; Orton, G. S.; Yanamandra-Fisher, P. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hueso, R.; Perez-Hoyos, S.; Sanchez-Lavega, A.] Univ Basque Country, Bilbao 48013, Spain.
[Simon-Miller, A. A.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hammel, HB (reprint author), Space Sci Inst, 4750 Walnut Ave,Suite 205, Boulder, CO 80301 USA.
EM hbh@alum.mit.edu
RI Fletcher, Leigh/D-6093-2011; Simon, Amy/C-8020-2012; Noll,
Keith/C-8447-2012; Perez-Hoyos, Santiago/L-7543-2014; Clarke,
John/C-8644-2013
OI Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186;
Perez-Hoyos, Santiago/0000-0002-2587-4682; Sanchez-Lavega,
Agustin/0000-0001-7355-1522; Hueso, Ricardo/0000-0003-0169-123X;
FU NASA [NAS 5-26555]; STScI [GO-12003, GO-12045]
FX This Letter is based on observations made with the NASA/ESA Hubble Space
Telescope, obtained 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. Analyses of these data
from programs GO-12003 and GO-12045 were supported by STScI under the
associated research grants. We commend and thank the STSCI staff and
management for their fortitude during these unusually challenging
observations. L.N.F. was supported by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory (California
Institute of Technology, Pasadena, CA).
NR 25
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 1
PY 2010
VL 715
IS 2
BP L150
EP L154
DI 10.1088/2041-8205/715/2/L150
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 608NU
UT WOS:000278591800019
ER
PT J
AU Sanchez-Lavega, A
Wesley, A
Orton, G
Hueso, R
Perez-Hoyos, S
Fletcher, LN
Yanamandra-Fisher, P
Legarreta, J
de Pater, I
Hammel, H
Simon-Miller, A
Gomez-Forrellad, JM
Ortiz, JL
Garcia-Melendo, E
Puetter, RC
Chodas, P
AF Sanchez-Lavega, A.
Wesley, A.
Orton, G.
Hueso, R.
Perez-Hoyos, S.
Fletcher, L. N.
Yanamandra-Fisher, P.
Legarreta, J.
de Pater, I.
Hammel, H.
Simon-Miller, A.
Gomez-Forrellad, J. M.
Ortiz, J. L.
Garcia-Melendo, E.
Puetter, R. C.
Chodas, P.
TI THE IMPACT OF A LARGE OBJECT ON JUPITER IN 2009 JULY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: general;
planets and satellites: individual (Jupiter)
ID SHOEMAKER-LEVY 9; SHORT-PERIOD COMETS; RECONSTRUCTION; EVOLUTION; RATES
AB On 2009 July 19, we observed a single, large impact on Jupiter at a planetocentric latitude of 55 degrees S. This and the Shoemaker-Levy 9 (SL9) impacts on Jupiter in 1994 are the only planetary-scale impacts ever observed. The 2009 impact had an entry trajectory in the opposite direction and with a lower incidence angle than that of SL9. Comparison of the initial aerosol cloud debris properties, spanning 4800 km east-west and 2500 km north-south, with those produced by the SL9 fragments and dynamical calculations of pre-impact orbit indicates that the impactor was most probably an icy body with a size of 0.5-1 km. The collision rate of events of this magnitude may be five to ten times more frequent than previously thought. The search for unpredicted impacts, such as the current one, could be best performed in 890 nm and K (2.03-2.36 mu m) filters in strong gaseous absorption, where the high-altitude aerosols are more reflective than Jupiter's primary clouds.
C1 [Sanchez-Lavega, A.; Hueso, R.; Perez-Hoyos, S.] Univ Basque Country, Dpto Fis Aplicada 1, Escuela Super Ingenieros, Bilbao 48013, Spain.
[Wesley, A.] Acquerra Pty Ltd, Murrumbateman, NSW 2582, Australia.
[Orton, G.; Yanamandra-Fisher, P.; Chodas, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fletcher, L. N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Legarreta, J.] Escuela Univ Ingn Tecn Ind, Bilbao 48012, Spain.
[de Pater, I.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Hammel, H.] Space Sci Inst, Boulder, CO 80301 USA.
[Simon-Miller, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gomez-Forrellad, J. M.; Garcia-Melendo, E.] Fundacio Observ Esteve Duran, Barcelona 08553, Spain.
[Ortiz, J. L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Puetter, R. C.] Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
RP Sanchez-Lavega, A (reprint author), Univ Basque Country, Dpto Fis Aplicada 1, Escuela Super Ingenieros, Alameda Urquijo S-N, Bilbao 48013, Spain.
EM agustin.sanchez@ehu.es
RI Fletcher, Leigh/D-6093-2011; Simon, Amy/C-8020-2012; Perez-Hoyos,
Santiago/L-7543-2014;
OI Fletcher, Leigh/0000-0001-5834-9588; Simon, Amy/0000-0003-4641-6186;
Perez-Hoyos, Santiago/0000-0002-2587-4682; LEGARRETA ETXAGIBEL, JON
JOSU/0000-0001-6501-2705; Sanchez-Lavega, Agustin/0000-0001-7355-1522;
Hueso, Ricardo/0000-0003-0169-123X
FU Spanish MEC [AYA2006-07735]; MICIIN [AYA2009-10701]; Grupos Gobierno
Vasco [IT-464-07]; NASA
FX This work was supported by the Spanish MEC AYA2006-07735 and MICIIN
AYA2009-10701 with FEDER and Grupos Gobierno Vasco IT-464-07. G.O. and
P.Y.F. acknowledge support from NASA grants to JPL. L.N.F. was supported
by NASA Postdoctoral Program at the Jet Propulsion Laboratory (Caltech,
USA). J.L.O. acknowledges AYA2008-06202-C03-01.
NR 26
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 1
PY 2010
VL 715
IS 2
BP L155
EP L159
DI 10.1088/2041-8205/715/2/L155
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 608NU
UT WOS:000278591800020
ER
PT J
AU Wu, JW
Evans, NJ
Shirley, YL
Knez, C
AF Wu, Jingwen
Evans, Neal J., II
Shirley, Yancy L.
Knez, Claudia
TI THE PROPERTIES OF MASSIVE, DENSE CLUMPS: MAPPING SURVEYS OF HCN AND CS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: formation; ISM: clouds; ISM: molecules; stars: formation;
submillimeter: ISM
ID STAR-FORMATION RATE; LUMINOUS INFRARED GALAXIES; MOLECULAR CLOUD CORES;
COMPACT HII-REGIONS; H-II REGIONS; PROTOSTELLAR CANDIDATES; PHYSICAL
CONDITIONS; CONTINUUM OBSERVATIONS; DUST CONTINUUM; OUTER GALAXY
AB We have mapped over 50 massive, dense clumps with four dense gas tracers: HCN J = 1-0 and 3-2; and CS J = 2-1 and 7-6 transitions. Spectral lines of optically thin H(13)CN 3-2 and C(34)S 5-4 were also obtained toward the map centers. These maps usually demonstrate single well-peaked distributions at our resolution, even with higher J transitions. The size, virial mass, surface density, and mean volume density within a well-defined angular size ( FWHM) were calculated from the contour maps for each transition. We found that transitions with higher effective density usually trace the more compact, inner part of the clumps but have larger linewidths, leading to an inverse linewidth-size relation using different tracers. The mean surface densities are 0.29, 0.33, 0.78, 1.09 g cm(-2) within FWHM contours of CS 2-1, HCN 1-0, HCN 3-2, and CS 7-6, respectively. We find no correlation of L(IR) with surface density and a possible inverse correlation with mean volume density, contrary to some theoretical expectations. Molecular line luminosities L'(mol) were derived for each transition. We see no evidence in the data for the relation between L'(mol) and mean density posited by modelers. The correlation between L'(mol) and the virial mass is roughly linear for each dense gas tracer. No obvious correlation was found between the line luminosity ratio and infrared luminosity, bolometric temperature, or the L(IR)/M(Vir) ratio. A nearly linear correlation was found between the infrared luminosity and the line luminosity of all dense gas tracers for these massive, dense clumps, with a lower cutoff in luminosity at L(IR) = 10(4.5) L(circle dot). The L(IR)-L'(HCN1-0) correlation agrees well with the one found in galaxies. These correlations indicate a constant star formation rate per unit mass from the scale of dense clumps to that of distant galaxies when the mass is measured for dense gas. These results support the suggestion that starburst galaxies may be understood as having a large fraction of gas in dense clumps.
C1 [Wu, Jingwen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Knez, Claudia] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Wu, JW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS78, Cambridge, MA 02138 USA.
EM jwu@cfa.harvard.edu; nje@astro.as.utexas.edu; yshirley@as.arizona.edu
FU Submillimeter Array of the Smithsonian Observatory; NSF [AST-0607793];
McDonald Observatory
FX We thank D. Narayanan and M. Krumholz for lively discussions that
illuminated their models. J.W. thanks the postdoctoral fellowship
support from the Submillimeter Array of the Smithsonian Observatory
while completing this work. This work was supported in part by NSF Grant
AST-0607793 and by McDonald Observatory.
NR 99
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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 JUN
PY 2010
VL 188
IS 2
BP 313
EP 357
DI 10.1088/0067-0049/188/2/313
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 613HG
UT WOS:000278969400001
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Allafort, A
Antolini, E
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Baughman, BM
Bechtol, K
Bellazzini, R
Belli, F
Berenji, B
Bisello, D
Blandford, RD
Bloom, ED
Bonamente, E
Bonnell, J
Borgland, AW
Bouvier, A
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Burnett, TH
Busetto, G
Buson, S
Caliandro, GA
Cameron, RA
Campana, R
Canadas, B
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Ceccanti, M
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Cillis, AN
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Corbet, R
Davis, DS
DeKlotz, M
den Hartog, PR
Dermer, CD
de Angelis, A
de Luca, A
de Palma, F
Digel, SW
Dormody, M
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Fabiani, D
Farnier, C
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giavitto, G
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grondin, MH
Grove, JE
Guillemot, L
Guiriec, S
Gustafsson, M
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hays, E
Healey, SE
Hill, AB
Horan, D
Hughes, RE
Iafrate, G
Johannesson, G
Johnson, AS
Johnson, RP
Johnson, TJ
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Kawai, N
Kerr, M
Knodlseder, J
Kocevski, D
Kuss, M
Lande, J
Landriu, D
Latronico, L
Lee, SH
Lemoine-Goumard, M
Lionetto, AM
Garde, ML
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Makeev, A
Marangelli, B
Marelli, M
Massaro, E
Mazziotta, MN
McConville, W
McEnery, JE
Michelson, PF
Minuti, M
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Mongelli, M
Monte, C
Monzani, ME
Moretti, E
Morselli, A
Moskalenko, IV
Murgia, S
Nakajima, H
Nakamori, T
Naumann-Godo, M
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paccagnella, A
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Pinchera, M
Piron, F
Porter, TA
Poupard, L
Raino, S
Rando, R
Ray, PS
Razzano, M
Razzaque, S
Rea, N
Reimer, A
Reimer, O
Reposeur, T
Ripken, J
Ritz, S
Rochester, LS
Rodriguez, AY
Romani, RW
Roth, M
Sadrozinski, HFW
Salvetti, D
Sanchez, D
Sander, A
Parkinson, PMS
Scargle, JD
Schalk, TL
Scolieri, G
Sgro, C
Shaw, MS
Siskind, EJ
Smith, DA
Smith, PD
Spandre, G
Spinelli, P
Starck, JL
Stephens, TE
Striani, E
Strickman, MS
Strong, AW
Suson, DJ
Tajima, H
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Tibolla, O
Tinebra, F
Torres, DF
Tosti, G
Tramacere, A
Uchiyama, Y
Usher, TL
Van Etten, A
Vasileiou, V
Vilchez, N
Vitale, V
Waite, AP
Wallace, E
Wang, P
Watters, K
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Antolini, E.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Baughman, B. M.
Bechtol, K.
Bellazzini, R.
Belli, F.
Berenji, B.
Bisello, D.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Bonnell, J.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Burnett, T. H.
Busetto, G.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Campana, R.
Canadas, B.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Ceccanti, M.
Cecchi, C.
Celik, Oe.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Cillis, A. N.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Corbet, R.
Davis, D. S.
DeKlotz, M.
den Hartog, P. R.
Dermer, C. D.
de Angelis, A.
de Luca, A.
de Palma, F.
Digel, S. W.
Dormody, M.
do Couto E Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Fabiani, D.
Farnier, C.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giavitto, G.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hays, E.
Healey, S. E.
Hill, A. B.
Horan, D.
Hughes, R. E.
Iafrate, G.
Johannesson, G.
Johnson, A. S.
Johnson, R. P.
Johnson, T. J.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kawai, N.
Kerr, M.
Knoedlseder, J.
Kocevski, D.
Kuss, M.
Lande, J.
Landriu, D.
Latronico, L.
Lee, S. -H.
Lemoine-Goumard, M.
Lionetto, A. M.
Garde, M. Llena
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Makeev, A.
Marangelli, B.
Marelli, M.
Massaro, E.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
Michelson, P. F.
Minuti, M.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Mongelli, M.
Monte, C.
Monzani, M. E.
Moretti, E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakajima, H.
Nakamori, T.
Naumann-Godo, M.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paccagnella, A.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Pinchera, M.
Piron, F.
Porter, T. A.
Poupard, L.
Raino, S.
Rando, R.
Ray, P. S.
Razzano, M.
Razzaque, S.
Rea, N.
Reimer, A.
Reimer, O.
Reposeur, T.
Ripken, J.
Ritz, S.
Rochester, L. S.
Rodriguez, A. Y.
Romani, R. W.
Roth, M.
Sadrozinski, H. F. -W.
Salvetti, D.
Sanchez, D.
Sander, A.
Parkinson, P. M. Saz
Scargle, J. D.
Schalk, T. L.
Scolieri, G.
Sgro, C.
Shaw, M. S.
Siskind, E. J.
Smith, D. A.
Smith, P. D.
Spandre, G.
Spinelli, P.
Starck, J. -L.
Stephens, T. E.
Striani, E.
Strickman, M. S.
Strong, A. W.
Suson, D. J.
Tajima, H.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Tibolla, O.
Tinebra, F.
Torres, D. F.
Tosti, G.
Tramacere, A.
Uchiyama, Y.
Usher, T. L.
Van Etten, A.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wallace, E.
Wang, P.
Watters, K.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
TI FERMI LARGE AREA TELESCOPE FIRST SOURCE CATALOG
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; gamma rays: general
ID GAMMA-RAY EMISSION; ACTIVE GALACTIC NUCLEI; SPECTRUM RADIO-SOURCES;
ALL-SKY SURVEY; SPACE-TELESCOPE; MILKY-WAY; LIKELIHOOD RATIO; EGRET
SOURCES; SUPERNOVA-REMNANTS; GLOBULAR-CLUSTER
AB We present a catalog of high-energy gamma-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), during the first 11 months of the science phase of the mission, which began on 2008 August 4. The First Fermi-LAT catalog (1FGL) contains 1451 sources detected and characterized in the 100 MeV to 100 GeV range. Source detection was based on the average flux over the 11 month period, and the threshold likelihood Test Statistic is 25, corresponding to a significance of just over 4 sigma. The 1FGL catalog includes source location regions, defined in terms of elliptical fits to the 95% confidence regions and power-law spectral fits as well as flux measurements in five energy bands for each source. In addition, monthly light curves are provided. Using a protocol defined before launch we have tested for several populations of gamma-ray sources among the sources in the catalog. For individual LAT-detected sources we provide firm identifications or plausible associations with sources in other astronomical catalogs. Identifications are based on correlated variability with counterparts at other wavelengths, or on spin or orbital periodicity. For the catalogs and association criteria that we have selected, 630 of the sources are unassociated. Care was taken to characterize the sensitivity of the results to the model of interstellar diffuse gamma-ray emission used to model the bright foreground, with the result that 161 sources at low Galactic latitudes and toward bright local interstellar clouds are flagged as having properties that are strongly dependent on the model or as potentially being due to incorrectly modeled structure in the Galactic diffuse emission.
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[Abdo, A. A.; Cheung, C. C.; Razzaque, S.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Van Etten, A.; Waite, A. P.; Wang, P.; Watters, K.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
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[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Atwood, W. B.; Dormody, M.; Johnson, R. P.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Schalk, T. L.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
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[Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.] Lund Observ, SE-22100 Lund, Sweden.
[Axelsson, M.; Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
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[Barbiellini, G.; Giavitto, G.; Iafrate, G.; Longo, F.; Moretti, E.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Giavitto, G.; Longo, F.; Moretti, E.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Bisello, D.; Busetto, G.; Buson, S.; Gustafsson, M.; Paccagnella, A.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Bisello, D.; Busetto, G.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Baughman, B. M.; Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Belli, F.; Canadas, B.; Lionetto, A. M.; Morselli, A.; Striani, E.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Belli, F.; Canadas, B.; Lionetto, A. M.; Striani, E.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Bonnell, J.; Celik, Oe.; Cillis, A. N.; Corbet, R.; Davis, D. S.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bonnell, J.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Bonnell, J.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Marangelli, B.; Mazziotta, M. N.; Mongelli, M.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Burnett, T. H.; Kerr, M.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Caliandro, G. A.; Rea, N.; Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Campana, R.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Caraveo, P. A.; Marelli, M.; Salvetti, D.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.; Corbet, R.; Davis, D. S.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cillis, A. N.] Parbellon IAFE, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[DeKlotz, M.] Stellar Solut Inc, Palo Alto, CA 94306 USA.
[de Angelis, A.; Frailis, M.; Guillemot, L.] 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.
[de Luca, A.] IUSS, I-27100 Pavia, Italy.
[Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.; Smith, D. A.] CEN Bordeaux Gradignan, UMR 5797, CNRS, IN2P3, F-33175 Gradignan, France.
[Dumora, D.; Grondin, M. -H.; Guillemot, L.; Lemoine-Goumard, M.; Lott, B.; Reposeur, T.; Smith, D. A.] Univ Bordeaux, CEN Bordeaux Gradignan, F-33175 Gradignan, France.
[Frailis, M.; Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Hadasch, D.; Torres, D. F.] ICREA, Barcelona, Spain.
[Hill, A. B.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Kawai, N.; Nakajima, H.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan.
[Kawai, N.] RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan.
[Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Massaro, E.; Tinebra, F.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Ohno, M.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Paccagnella, A.] Univ Padua, Dipartimento Ingn Informaz, I-35131 Padua, Italy.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Scargle, J. D.; Stephens, T. E.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Scolieri, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stephens, T. E.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Ylinen, T.] Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM jean.ballet@cea.fr; digel@stanford.edu; knodlseder@cesr.fr
RI Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; Funk, Stefan/B-7629-2015; Campana,
Riccardo/F-5272-2015; Rea, Nanda/I-2853-2015; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Johannesson,
Gudlaugur/O-8741-2015; 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; Ozaki, Masanobu/K-1165-2013; 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; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Saz Parkinson, Pablo
Miguel/I-7980-2013;
OI Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins,
Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; De
Luca, Andrea/0000-0001-6739-687X; Giroletti,
Marcello/0000-0002-8657-8852; Moretti, Elena/0000-0001-5477-9097;
Stephens, Thomas/0000-0003-3065-6871; Iafrate,
Giulia/0000-0002-6185-8292; Sgro', Carmelo/0000-0001-5676-6214;
Giordano, Francesco/0000-0002-8651-2394; SPINELLI,
Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; 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; Hill, Adam/0000-0003-3470-4834; Bastieri,
Denis/0000-0002-6954-8862; Funk, Stefan/0000-0002-2012-0080; Campana,
Riccardo/0000-0002-4794-5453; Rea, Nanda/0000-0003-2177-6388; Loparco,
Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395;
Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; 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; Reimer, Olaf/0000-0001-6953-1385;
Berenji, Bijan/0000-0002-4551-772X; Gasparrini,
Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793;
Baldini, Luca/0000-0002-9785-7726; Ray, Paul/0000-0002-5297-5278;
Marelli, Martino/0000-0002-8017-0338
FU K. A. Wallenberg Foundation; European Community [ERC-StG-200911];
International Doctorate on Astroparticle Physics (IDAPP) program;
National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; Agenzia Spaziale Italiana and the
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; Swedish Research Council; Swedish National Space Board in
Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National
d'Etudes Spatiales in France; CEA; CNES; Universite Paris Diderot
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-200911
from the European Community.; Partially supported by the International
Doctorate on Astroparticle Physics (IDAPP) program.; The Fermi-LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and the
operation of the LAT as well as scientific data analysis. These include
the National Aeronautics and Space Administration and the Department of
Energy in the United States, the Commissariat a l'Energie 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.
WallenbergFoundation, the Swedish Research Council and the Swedish
National Space Board in Sweden.; Additional support for science analysis
during the operations phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France. The catalog work used a cluster of computing nodes
at Saclay funded by CEA, CNES, and Universite Paris Diderot.
NR 101
TC 577
Z9 578
U1 3
U2 37
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2010
VL 188
IS 2
BP 405
EP 436
DI 10.1088/0067-0049/188/2/405
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 613HG
UT WOS:000278969400004
ER
PT J
AU Cotton, WD
Ragland, S
Pluzhnik, EA
Danchi, WC
Traub, WA
Willson, LA
Lacasse, MG
AF Cotton, W. D.
Ragland, S.
Pluzhnik, E. A.
Danchi, W. C.
Traub, W. A.
Willson, L. A.
Lacasse, M. G.
TI SiO MASERS IN ASYMMETRIC MIRAS. IV. chi CYGNI, R AQUILAE, R LEO MINORIS,
RU HERCULIS, U HERCULIS, AND U ORIONIS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE radio lines: stars; stars: AGB and post-AGB; stars: atmospheres
ID LATE-TYPE STARS; GIANT BRANCH STARS; VARIABLE-STARS; WATER MASERS; RADIO
PHOTOSPHERES; ANGULAR DIAMETERS; VLBA OBSERVATIONS; EVOLVED STARS;
STELLAR IMAGE; IK TAURI
AB This is the fourth paper in a series of multi-epoch observations at 7 mm wavelength of the SiO masers in several asymptotic giant branch stars from a sample of Mira variable stars showing evidence of asymmetric structure in the infrared. These stars have been observed interferometrically in the infrared by IOTA and with VLBA measurements of the SiO masers. In this paper, we present the observations of chi Cygni (chi Cyg), R Aquilae (R Aql), R Leo Minoris (R LMi), RU Herculis (RU Her), U Herculis (U Her), and U Orionis (U Ori). Several radial features with velocity gradients were observed, all with velocities close to systemic furthest from the star and redshifted closer to the stellar surface. Systemic velocities are estimated for several of the stars. No compelling evidence of asymmetry is seen in the maser distributions. All maser rings are approximately twice the near-IR uniform disk diameter and are comparable in size to the extended molecular envelope when such measurements are available.
C1 [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA.
[Pluzhnik, E. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Willson, L. A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA.
[Lacasse, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
EM bcotton@nrao.edu
FU NSF [AST-0456047]
FX We acknowledge support from NSF of the IOTA observations through grant
AST-0456047. The authors thank the anonymous referee for comments
leading to an improved paper.
NR 50
TC 10
Z9 10
U1 0
U2 1
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 JUN
PY 2010
VL 188
IS 2
BP 506
EP 525
DI 10.1088/0067-0049/188/2/506
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 613HG
UT WOS:000278969400010
ER
PT J
AU Duncan, BN
Yoshida, Y
Olson, JR
Sillman, S
Martin, RV
Lamsal, L
Hu, YT
Pickering, KE
Retscher, C
Allen, DJ
Crawford, JH
AF Duncan, Bryan N.
Yoshida, Yasuko
Olson, Jennifer R.
Sillman, Sanford
Martin, Randall V.
Lamsal, Lok
Hu, Yongtao
Pickering, Kenneth E.
Retscher, Christian
Allen, Dale J.
Crawford, James H.
TI Application of OMI observations to a space-based indicator of NOx and
VOC controls on surface ozone formation
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Surface ozone; Air quality indicator; OMI; HCHO; NO2
ID EASTERN UNITED-STATES; ISOPRENE EMISSIONS; NITROGEN-OXIDES; AIR-QUALITY;
PRECURSOR RELATIONSHIPS; NEW-YORK; URBAN; PHOTOCHEMISTRY; SENSITIVITY;
REDUCTIONS
AB We investigated variations in the relative sensitivity of surface ozone formation in summer to precursor species concentrations of volatile organic compounds (VOCs) and nitrogen oxides (NOx) as inferred from the ratio of the tropospheric columns of formaldehyde to nitrogen dioxide (the "Ratio") from the Aura Ozone Monitoring Instrument (OMI). Our modeling study suggests that ozone formation decreases with reductions in VOCs at Ratios <1 and NOx at Ratios >2; both NOx and VOC reductions may decrease ozone formation for Ratios between 1 and 2. Using this criteria, the OMI data indicate that ozone formation became: 1. more sensitive to NOx over most of the United States from 2005 to 2007 because of the substantial decrease in NOx emissions, primarily from stationary sources, and the concomitant decrease in the tropospheric column of NO2, and 2. more sensitive to NOx with increasing temperature, in part because emissions of highly reactive, biogenic isoprene increase with temperature, thus increasing the total VOC reactivity. In cities with relatively low isoprene emissions (e.g., Chicago), the data clearly indicate that ozone formation became more sensitive to NOx from 2005 to 2007. In cities with relatively high isoprene emissions (e.g., Atlanta), we found that the increase in the Ratio due to decreasing NOx emissions was not obvious as this signal was convolved with variations in the Ratio associated with the temperature dependence of isoprene emissions and, consequently, the formaldehyde concentration. Published by Elsevier Ltd.
C1 [Duncan, Bryan N.; Yoshida, Yasuko; Pickering, Kenneth E.; Retscher, Christian] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA.
[Yoshida, Yasuko; Retscher, Christian] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
[Olson, Jennifer R.; Crawford, James H.] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA.
[Sillman, Sanford] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Martin, Randall V.; Lamsal, Lok] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hu, Yongtao] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA.
[Allen, Dale J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 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; Pickering, Kenneth/E-6274-2012; Lamsal,
Lok/G-4781-2012; Pfister, Gabriele/A-9349-2008; Crawford,
James/L-6632-2013; Martin, Randall/C-1205-2014; Hu, Yongtao/H-7543-2016;
Allen, Dale/F-7168-2010;
OI Crawford, James/0000-0002-6982-0934; Martin,
Randall/0000-0003-2632-8402; Hu, Yongtao/0000-0002-5161-0592; Allen,
Dale/0000-0003-3305-9669; Sillman, Sanford/0000-0001-6250-1191
FU NASA
FX This work was supported by the NASA's Earth Science Research Program.
NR 55
TC 47
Z9 51
U1 10
U2 88
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 JUN
PY 2010
VL 44
IS 18
BP 2213
EP 2223
DI 10.1016/j.atmosenv.2010.03.010
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 613ON
UT WOS:000278988700006
ER
PT J
AU Fishman, J
Creilson, JK
Parker, PA
Ainsworth, EA
Vining, GG
Szarka, J
Booker, FL
Xu, XJ
AF Fishman, Jack
Creilson, John K.
Parker, Peter A.
Ainsworth, Elizabeth A.
Vining, G. Geoffrey
Szarka, John
Booker, Fitzgerald L.
Xu, Xiaojing
TI An investigation of widespread ozone damage to the soybean crop in the
upper Midwest determined from ground-based and satellite measurements
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air pollution; Crop damage; Ozone; Remote sensing; Soybean; Yield
ID AIR-QUALITY FORECASTS; TROPOSPHERIC OZONE; UNITED-STATES; SURFACE OZONE;
YIELD; METAANALYSIS; POLLUTION; EXPOSURE; GROWTH; RESIDUALS
AB Elevated concentrations of ground-level ozone (O(3)) are frequently measured over farmland regions in many parts of the world. While numerous experimental studies show that O(3) can significantly decrease crop productivity, independent verifications of yield losses at current ambient O(3) concentrations in rural locations are sparse. In this study, soybean crop yield data during a 5-year period over the Midwest of the United States were combined with ground and satellite O(3) measurements to provide evidence that yield losses on the order of 10% could be estimated through the use of a multiple linear regression model. Yield loss trends based on both conventional ground-based instrumentation and satellite-derived tropospheric O(3) measurements were statistically significant and were consistent with results obtained from open-top chamber experiments and an open-air experimental facility (SoyFACE, Soybean Free Air Concentration Enrichment) in central Illinois. Our analysis suggests that such losses are a relatively new phenomenon due to the increase in background tropospheric O(3) levels over recent decades. Extrapolation of these findings supports previous studies that estimate the global economic loss to the farming community of more than $10 billion annually. Published by Elsevier Ltd.
C1 [Fishman, Jack; Creilson, John K.; Xu, Xiaojing] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Creilson, John K.] Univ Massachusetts, Dept Geosci, Amherst, MA 01003 USA.
[Parker, Peter A.] NASA, Langley Res Ctr, Syst Engn Directorate, Hampton, VA 23681 USA.
[Ainsworth, Elizabeth A.] Univ Illinois, USDA, ARS, Photosynth Res Unit, Urbana, IL 61801 USA.
[Ainsworth, Elizabeth A.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
[Vining, G. Geoffrey; Szarka, John] Virginia Polytech Inst & State Univ, Dept Stat, Blacksburg, VA 24061 USA.
[Booker, Fitzgerald L.] N Carolina State Univ, USDA, ARS, Plant Sci Res Unit, Raleigh, NC 27695 USA.
[Booker, Fitzgerald L.] N Carolina State Univ, Dept Crop Sci, Raleigh, NC 27695 USA.
RP Fishman, J (reprint author), NASA, Langley Res Ctr, Sci Directorate, Mail Stop 401A, Hampton, VA 23681 USA.
EM jack.fishman@nasa.gov
NR 41
TC 45
Z9 45
U1 1
U2 33
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 JUN
PY 2010
VL 44
IS 18
BP 2248
EP 2256
DI 10.1016/j.atmosenv.2010.01.015
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 613ON
UT WOS:000278988700010
ER
PT J
AU Gauthier, ML
Petersen, WA
Carey, LD
AF Gauthier, Michael L.
Petersen, Walter A.
Carey, Lawrence D.
TI Cell mergers and their impact on cloud-to-ground lightning over the
Houston area
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Lightning; Radar; Cell merger
ID MAJOR URBAN AREAS; SUMMER SEASON; RADAR; PRECIPITATION; CONVECTION;
SATELLITE; CUMULUS; ISLAND; TRMM
AB A previous hypothesis advanced from observational studies such as METROMEX suggests that the intensity, frequency, and organization of cumulus convection may be impacted by the forcing of enhanced merger activity downstream of urban zones. A resulting corollary is that cities may exert an indirect anthropogenic "forcing" of parameters related to convection and associated phenomena such as lightning and precipitation. This paper investigates the urban-merger hypothesis by examining the role of convective cell mergers on the existence and persistence of the Houston lightning "anomaly", a local maximum in cloud-to-ground (CG) lightning activity documented to exist over and east of Houston.
Using eight summer seasons of peak columnar radar reflectivity. CG lightning data and a cell-tracking algorithm, a two-dimensional cell merger climatology is created for portions of Eastern Texas and Louisiana. Results from the tracking and analysis of over 3.8 million cells indicate that merger-driven enhancements in convection induce a positive response (046%) in ground flash densities throughout the domain, with areas of enhanced lightning typically being co-located with areas of enhanced merger activity. However, while mergers over the Houston area (relative to elsewhere in the domain) do result in more vigorous convective cells that produce larger CG flash densities, we find that CG lightning contributions due to mergers are distributed similarly throughout the domain. Hence while we demonstrate that cell mergers do greatly impact the production of lightning, the urban cell merger hypothesis does not uniquely explain the presence of a local lightning maximum near and downstream of Houston. Published by Elsevier B.V.
C1 [Gauthier, Michael L.] USAF Acad, Dept Phys, Colorado Springs, CO 80840 USA.
[Petersen, Walter A.] NASA Marshall Space Flight Ctr, NSSTC Earth Sci Off VP61, Huntsville, AL 35804 USA.
[Carey, Lawrence D.] Univ Alabama, Natl Space Sci & Technol Ctr, Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
RP Gauthier, ML (reprint author), USAF Acad, Dept Phys, 2354 Fairchild Hall,Suite 2A29, Colorado Springs, CO 80840 USA.
EM Michael.Gauthier@USAFA.edu
FU U.S. Air Force Academy through the Air Force Institute of Technology;
NASA; NSF [ATM-0442011]
FX This research was supported by funding from the U.S. Air Force Academy
through the Air Force Institute of Technology (MLG), NASA's Earth
Sciences Program (WAP), and NSF grant ATM-0442011 (LDC). The views
expressed in this paper are those of the authors and do not reflect the
official policy or position of the U.S. Air Force, Department of
Defense, or the U.S. Government.
NR 28
TC 7
Z9 9
U1 1
U2 3
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 JUN
PY 2010
VL 96
IS 4
BP 626
EP 632
DI 10.1016/j.atmosres.2010.02.010
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 607BV
UT WOS:000278474200013
ER
PT J
AU Johnston, SL
Campbell, MR
Scheuring, R
Feiveson, AH
AF Johnston, Smith L.
Campbell, Mark R.
Scheuring, Rick
Feiveson, Alan H.
TI Risk of Herniated Nucleus Pulposus Among US Astronauts
SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE
LA English
DT Article
DE spaceflight; back pain; back injury; cervical injury; lumbar injury;
disc disease; microgravity; weightlessness
ID FIGHTER PILOTS; INTERVERTEBRAL-DISK; BACK-PAIN; GZ FORCES; BED REST;
MICROGRAVITY; INJURY; SPINE; MRI; DEGENERATION
AB JOHNSTON SL, CAMPBELL MR, SCHEURING R, FEIVESON AH. Risk of herniated nucleus pulposus among U.S. astronauts. Aviat Space Environ Med 2010; 81:566-74.
Introduction: Astronauts have complained of back pain occurring during spaceflight, presumably due to the elongation of the spine from the lack of gravity. Herniated nucleus pulposus (HNP) is known to occur in aviators exposed to high G, and has been diagnosed in several astronauts in the immediate post-spaceflight period. It is unknown whether astronauts exposed to microgravity are at added risk for developing HNP in the post-spaceflight period due to possible in-flight intervertebral disc changes. Methods: For a preset study period, incidence rates of HNP were compared between the U.S. astronaut population and a matched control population not involved in spaceflight using the Longitudinal Study of Astronaut Health database. Using a Weibull survival model, time trends of the risk of HNP prior to and after spaceflight were compared within the astronaut group. HNP incidences in other populations that have previously been reported in the literature were also compared with results in this study. Results: The incidence of HNP was 4.3 times higher in the U.S. astronaut population (N = 321) compared to matched controls (N = 983) not involved in spaceflight. For astronauts, there was relatively more HNP in the cervical region of the spine (18 of 44) than for controls (3 of 35); however, there was no clear increase of HNP incidence in those astronauts who were high performance jet aircraft pilots. There was evidence suggesting that the risk is increased immediately after spaceflight. Conclusions: Astronauts are at higher risk of incurring HNP especially immediately following spaceflight.
C1 [Johnston, Smith L.; Scheuring, Rick; Feiveson, Alan H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Campbell, MR (reprint author), 420 DeShong,300, Paris, TX 75460 USA.
EM mcamp@1starnet.com
NR 38
TC 34
Z9 37
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 JUN
PY 2010
VL 81
IS 6
BP 566
EP 574
DI 10.3357/ASEM.2427.2010
PG 9
WC Public, Environmental & Occupational Health; Medicine, General &
Internal; Sport Sciences
SC Public, Environmental & Occupational Health; General & Internal
Medicine; Sport Sciences
GA 604VA
UT WOS:000278305400006
PM 20540448
ER
PT J
AU Lee, TF
Nelson, CS
Dills, P
Riishojgaard, LP
Jones, A
Li, L
Miller, S
Flynn, LE
Jedlovec, G
McCarty, W
Hoffman, C
McWilliams, G
AF Lee, Thomas F.
Nelson, Craig S.
Dills, Patrick
Riishojgaard, Lars Peter
Jones, Andy
Li, Li
Miller, Steven
Flynn, Lawrence E.
Jedlovec, Gary
McCarty, William
Hoffman, Carl
McWilliams, Gary
TI NPOESS Next-Generation Operational Global Earth Observations
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID IRRADIANCE MONITOR; INSTRUMENT DESIGN; OBSERVING SYSTEM; MODIS; AIRS;
CAPABILITIES; IMAGERY; SENSOR
AB The United States is merging its two polar-orbiting operational environmental satellite programs operated by the Department of Commerce and the Department of Defense into a single system, which is called the National Polar-orbiting Operational Environmental Satellite System (NPOESS). During the next decade, NPOESS will provide global operational data to meet many of the needs of weather forecasters, climate researchers, and global decision makers for remotely sensed Earth science data and global environmental monitoring. The NPOESS Preparatory Project (NPP) will be launched in 2011 as a precursor to NPOESS to reduce final development risks for NPOESS and to provide continuity of global imaging and atmospheric sounding data from the National Aeronautics and Space Administration (NASA) Earth Observing System (EOS) missions. Beginning in 2014, NPOESS spacecraft will be launched into an afternoon orbit and in 2016 into an early-morning orbit to provide significantly improved operational capabilities and benefits to satisfy critical civil and national security requirements for space-based, remotely sensed environmental data. The European Organisation for the Exploitation of Meteorological Satellites (EUMETSAT) Meteorological Operation (MetOp) spacecraft will complement NPOESS in a midmorning orbit. The joint constellation will provide global coverage with a data refresh rate of approximately four hours. NPOESS will observe more phenomena simultaneously from space and deliver a data volume significantly greater than its operational predecessors with substantially improved data delivery to users. Higher-resolution (spatial and spectral) and more accurate imaging and atmospheric sounding data will enable improvements in short-to medium-range weather forecasts. Multispectral and hyperspectral instruments on NPOESS will provide global imagery and sounding products useful to the forecaster that are complementary to those available from geostationary satellites. NPOESS will support the operational needs of meteorological, oceanographic, environmental, climatic, and space environmental remote sensing programs and provide continuity of data for climate researchers. This article that describes NPOESS was completed and accepted for publication prior to the White House decision in February 2010 ordering a major restructuring of the NPOESS program. The Department of Commerce will now assume primary responsibility for the afternoon polar-orbiting operational environmental satellite orbit and the Department of Defense will take primary responsibility for the early morning orbit. However, NPP, as described in this article, is still scheduled to be launched in 2011. Several of the instruments and program elements described in this article are also likely to be carried forward into future U. S. polar-orbiting operational environmental satellite missions.
C1 [Lee, Thomas F.; Li, Li] USN, Res Lab, Monterey, CA 93943 USA.
[Nelson, Craig S.] Riverside Technol Inc, Silver Spring, MD USA.
[Dills, Patrick] Cooperat Program Operat Meteorol Educ & Training, Boulder, CO USA.
[Riishojgaard, Lars Peter] NOAA, Joint Ctr Satellite Data Assimilat, Ctr Sci, Camp Springs, MD USA.
[Jones, Andy; Miller, Steven] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Flynn, Lawrence E.] NOAA, NESDIS, Ctr Satellite Applicat & Res, Camp Springs, MD USA.
[Jedlovec, Gary] NASA, Global Hydrol & Climate Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Jedlovec, Gary] NASA, Short Term Predict Res & Transit Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[McCarty, William] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McCarty, William] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Hoffman, Carl; McWilliams, Gary] NPOESS Integrated Program Off, Silver Spring, MD USA.
RP Lee, TF (reprint author), USN, Res Lab, 7 Grace Hopper Ave,Stop 2, Monterey, CA 93943 USA.
EM thomas.lee@nrlmry.navy.mil
RI Flynn, Lawrence/B-6321-2009; Jones, Andrew/D-3291-2012; McCarty,
Will/E-9359-2012
OI Flynn, Lawrence/0000-0001-6856-2614; Jones, Andrew/0000-0002-0995-4957;
FU National Polar-orbiting Operational Environmental Satellite System
Integrated Program Office, Silver Spring, Maryland; Office of Naval
Research [PE-0602435N]; Navy at Space and Naval Warfare Systems Command
[PEO C4I, PMW-120, PE-0603207N]
FX The support of the research sponsors 1) the National Polar-orbiting
Operational Environmental Satellite System Integrated Program Office
located in Silver Spring, Maryland; 2) the Office of Naval Research
under Program Element PE-0602435N; and 3) the Oceanographer of the Navy
through the program office at the Space and Naval Warfare Systems
Command, PEO C4I and PMW-120 under Program Element PE-0603207N, is
gratefully acknowledged. We thank Jeffrey Hawkins from NRL and John
Furgerson from the IPO for several insightful suggestions.
NR 30
TC 19
Z9 19
U1 0
U2 6
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 JUN
PY 2010
VL 91
IS 6
BP 727
EP +
DI 10.1175/2009BAMS2953.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 628HT
UT WOS:000280107300002
ER
PT J
AU Mclain, JS
AF Mclain, Jeffrey S.
TI MANAGING THE TUOLUMNE RIVER FOR SALMONIDS: ASSESSMENT OF THE 1995
SETTLEMENT AGREEMENT
SO CALIFORNIA FISH AND GAME
LA English
DT Article
DE California; Chinook salmon; Oncorhynchus mykiss; Oncorhynchus
tshawytscha; San Joaquin River; steelhead; Tuolumne River; Yosemite
AB The Tuolumne River originates at elevations over 3,900 meters in Yosemite Valley, California along the Western Sierra and is the largest tributary to the San Joaquin River of the Central Valley, draining an area of approximately 2,500 km(2). The Tuolumne River was once home to a healthy population of spring and fall-run Chinook salmon, Oncorhynchus tshawytscha, the spring-run likely ascending upstream as high as the boundary of Yosemite National Park, at an elevation of nearly 760 meters. Although historical records of the presence of Central Valley steelhead, Oncorhynchus mykiss are poor, they were believed to be well distributed in the Tuolumne River and its smaller tributaries. A series of dams for water supply, hydroelectric generation, and flood control were constructed starting in the 1890s. These dams cut off access by native anadromous fish to as much as 90 h. of their spawning habitat. In 1996 the Federal Energy Regulatory Commission issued an order amending a 1964 license, which included a 1995 Settlement Agreement. The 1995 Settlement Agreement designated a Technical Advisory Committee to oversee implementation of the agreement and its requirements. A review of the hydrographs of the Tuolumne River during the first 8 years under the Settlement Agreement revealed they were significantly different in timing and magnitude than recommended by resource agencies. This paper discusses management implications of the Settlement Agreement, and also offers recommendations for improvement.
C1 [Mclain, Jeffrey S.] US Fish & Wildlife Serv, Sacramento, CA 95825 USA.
RP Mclain, JS (reprint author), Natl Marine Fisheries Serv, 650 Capitol Mall, Sacramento, CA 95814 USA.
EM Jeff.McLain@noaa.gov
NR 14
TC 0
Z9 0
U1 4
U2 10
PU CALIFORNIA FISH AND GAME EDITOR
PI SACRAMENTO
PA 1416 NINTH ST, SACRAMENTO, CA 95814 USA
SN 0008-1078
J9 CALIF FISH GAME
JI Calif. Fish Game
PD SUM
PY 2010
VL 96
IS 3
BP 173
EP 187
PG 15
WC Fisheries; Zoology
SC Fisheries; Zoology
GA 703OE
UT WOS:000285987300001
ER
PT J
AU Kamikawa, DJ
Stevenson, DE
AF Kamikawa, Daniel J.
Stevenson, Duane E.
TI NEW RECORDS OF ALDROVANDIA OLEOSA (NOTACANTHIFORMES: HALOSAURIDAE) FROM
THE EASTERN NORTH PACIFIC OCEAN
SO CALIFORNIA FISH AND GAME
LA English
DT Editorial Material
C1 [Kamikawa, Daniel J.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Fisheries Resource Anal & Monitoring Div, Newport, OR 97365 USA.
[Stevenson, Duane E.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Assessment & Conservat Engn Div, Seattle, WA 98115 USA.
RP Kamikawa, DJ (reprint author), Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Fisheries Resource Anal & Monitoring Div, 2032 SE Oregon State Univ Dr, Newport, OR 97365 USA.
EM Dan.Kamikawa@noaa.gov
NR 7
TC 1
Z9 1
U1 0
U2 1
PU CALIFORNIA FISH AND GAME EDITOR
PI SACRAMENTO
PA 1416 NINTH ST, SACRAMENTO, CA 95814 USA
SN 0008-1078
J9 CALIF FISH GAME
JI Calif. Fish Game
PD SUM
PY 2010
VL 96
IS 3
BP 216
EP 220
PG 5
WC Fisheries; Zoology
SC Fisheries; Zoology
GA 703OE
UT WOS:000285987300005
ER
PT J
AU Zhang, P
Imhoff, ML
Wolfe, RE
Bounoua, L
AF Zhang, Ping
Imhoff, Marc L.
Wolfe, Robert E.
Bounoua, Lahouari
TI Characterizing urban heat islands of global settlements using MODIS and
nighttime lights products
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID LAND-SURFACE TEMPERATURE; MULTISENSOR DATA; CLIMATE MODEL; TROPICAL
CITY; PARAMETERS; VEGETATION; CITIES; INTENSITY; FEATURES; INDEXES
AB Impervious surface area (ISA) from the National Geophysical Data Center (NGDC) and land surface temperature (LST) from the Moderate Resolution Imaging Spectroradiometer (MODIS) averaged over three annual cycles (2003-2005) are used in a spatial analysis to assess the urban heat island (UHI) signature on LST amplitude and its relationship with development intensity, size, and ecological setting for more than 3000 urban settlements globally. Development intensity zones based on fractional ISA are defined for each urban area emanating outward from the urban core to the nearby nonurban rural areas and used to stratify sampling for LST. Sampling is further constrained by biome type and elevation data to ensure objective intercomparisons between zones and between cities in different biomes. We find that the ecological context and settlement size significantly influence the amplitude of summer daytime UHI. Globally, an average of 3.8 degrees C UHI is found in cities built in biomes dominated by forests; 1.9 degrees C UHI in cities embedded in grass-shrubs biomes; and only a weak UHI or sometimes an urban heat sink (UHS) in cities in arid and semi-arid biomes. Overall, the amplitude of the UHI is negatively correlated (R = -0.66) with the difference in vegetation density between urban and rural zones represented by the MODIS normalized difference vegetation index (NDVI). Globally averaged, the daytime UHI amplitude for all settlements is 2.6 degrees C in summer and 1.4 degrees C in winter. Globally, the average summer daytime UHI is 4.7 degrees C for settlements larger than 500 km(2) compared with 2.5 degrees C for settlements smaller than 50 km(2) and larger than 10 km(2). The stratification of cities by size indicates that the aggregated amount of ISA is the primary driver of UHI amplitude, with variations between ecological contexts and latitudinal zones. More than 60% of the total LST variance is explained by ISA for urban settlements within forests at mid to high latitudes. This percentage will increase to more than 80% when only settlements in the US are examined.
C1 [Zhang, Ping] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Ping] Earth Resource Technol Inc, Annapolis Jct, MD 20701 USA.
[Imhoff, Marc L.; Wolfe, Robert E.; Bounoua, Lahouari] NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Zhang, P (reprint author), NASA, Hydrospher & Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Ping.zhang-1@nasa.gov
RI Zhang, Ping/D-7257-2012; Wolfe, Robert/E-1485-2012
OI Wolfe, Robert/0000-0002-0915-1855
NR 43
TC 26
Z9 28
U1 1
U2 15
PU CANADIAN AERONAUTICS & SPACE INST
PI KANATA
PA 350 TERRY FOX DR, STE 104, KANATA, ON K2K 2W5, CANADA
SN 0703-8992
EI 1712-7971
J9 CAN J REMOTE SENS
JI Can. J. Remote Sens.
PD JUN
PY 2010
VL 36
IS 3
SI SI
BP 185
EP 196
PG 12
WC Remote Sensing
SC Remote Sensing
GA 681VZ
UT WOS:000284352700004
ER
PT J
AU Hwang, JS
Kim, HR
Suh, M
Taylor, PT
Kutina, J
Hu, WJ
AF Hwang, Jong Sun
Kim, Hyung Rae
Suh, Mancheol
Taylor, Patrick T.
Kutina, Jan
Hu Wei-Jian
TI Long-wavelength geopotential fields study of East Asia from satellite
data
SO CHINESE JOURNAL OF GEOPHYSICS-CHINESE EDITION
LA Chinese
DT Article
DE Satellite observations; Gravity; magnetic; GRACE; CHAMP; East Asia
ID SPHERICAL-EARTH GRAVITY; ANOMALY CORRELATIONS
AB Kutina et al. proposed the existence of a large fracture zone extending from northern China across the Yellow sea, Korean peninsula, East Sea (a. k. a., Sea of Japan) and on to Honshu Island, Japan, which they called the 'Forty-North Fracture Zone'. We investigated this proposed large tectonic feature from making large-scale regional gravity and magnetic anomaly maps by using GRACE and CHAMP satellite potential field data. The regional study area extended from 24 degrees to 56 degrees north latitude and 90 degrees E to 150 degrees E and the detailed area from 32 degrees N to 42 degrees N and 122 degrees E to 132 degrees E. Recently, Taylor et al. constructed the magnetic anomaly maps directly from CHAMP track data collected between June and December, 2005 after removing the core-generated and external fields from the measurements and then reduced these data to the pole to seek any tectonic features. They also produced a mathematical model using available geologic and geophysical information for their interpretation. In this study, we augmented a gravity anomaly field map from the GRACE data measured during a month of October, 2003. The measured potential differences data were converted to vertical gravity anomaly values using Gauss-Legendre quadrature method, and long wavelengths over 1100 km of the anomalies were removed by subtracting the latest EGM96 field to compare with the magnetic data. A curious latitudinal structure was found in both gravity and magnetic anomaly fields that showed an inverse correlation. A forward modeling was performed from using a spherical prism model and the wavenumber correlation analysis between these two anomaly fields was made to delineate the common features over the study area, and these results were discussed in relation to the existence of the 'Forty-North Fracture Zone' in the East Asian region.
C1 [Hwang, Jong Sun; Taylor, Patrick T.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
[Hwang, Jong Sun] Korea Inst Geosci & Mineral Resources, Petr & Marine Resources Res Div, Taejon 305350, South Korea.
[Kim, Hyung Rae; Suh, Mancheol] Kongju Nat Univ, Dept Geoenvironm Sci, Kong Ju 314701, Chungnam, South Korea.
[Kutina, Jan] American Univ, Dept Chem, Lab Global Tecton & Metallogeny, Washington, DC 20016 USA.
[Hu Wei-Jian] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Petr Resources Res, Beijing 100029, Peoples R China.
RP Hwang, JS (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
EM hwang1975@gmail.com; kimhr@kongju.ac.kr
RI Taylor, Patrick/D-4707-2012; Hu, Weijian/A-2594-2015
OI Taylor, Patrick/0000-0002-1212-9384;
NR 19
TC 0
Z9 0
U1 0
U2 6
PU SCIENCE CHINA PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 0001-5733
J9 CHINESE J GEOPHYS-CH
JI Chinese J. Geophys.-Chinese Ed.
PD JUN
PY 2010
VL 53
IS 6
BP 1327
EP 1335
DI 10.3969/j.issn.0001-5733.2010.06.011
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 619QT
UT WOS:000279445500011
ER
PT J
AU Gerson, AL
Bruck, HA
Hopkins, AR
Segal, KN
AF Gerson, Alan L.
Bruck, Hugh A.
Hopkins, Alan R.
Segal, Kenneth N.
TI Curing effects of single-wall carbon nanotube reinforcement on
mechanical properties of filled epoxy adhesives
SO COMPOSITES PART A-APPLIED SCIENCE AND MANUFACTURING
LA English
DT Article
DE Nano-structures; Mechanical properties; Thermosetting resin; Cure
ID POLYMER NANOCOMPOSITES; COMPOSITES; MODEL
AB Enhancing epoxy adhesives using nanoscale fillers requires understanding processing-structure-property relationships as a function of nanoscale filler loading. In particular, the effects of adding nanoscale reinforcement to filled epoxies, such as those qualified for space applications, have yet to be characterized. In this effort, the addition of single-walled carbon nanotubes (SWNTs) to Hysol 9309.2 epoxy was investigated using a multi-scale mechanical characterization approach. Effects of SWNTs on the kinetics of epoxy curing were characterized and modeled using macromechanical dynamic mechanical analysis (DMA). Adhesion between SWNTs and microfiber reinforcement was identified with scanning electron microscope (SEM), and effects of SWNTs on mechanical properties of the filled epoxy were quantified using micromechanical tensile testing. Effects of SWNT reinforcement on mechanical behavior of the epoxy matrix were also characterized using nanomechanical characterization. This multi-scale mechanical characterization enabled the effects of SWNTs to be isolated from the epoxy and filler phases inherent in the adhesive. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Bruck, Hugh A.] Aerosp Corp, Space Mat Lab, Dept Mat Sci, Los Angeles, CA 90009 USA.
[Gerson, Alan L.] Univ Maryland, Dept Mech Engn, College Pk, MD 20742 USA.
[Hopkins, Alan R.; Segal, Kenneth N.] NASA, Goddard Space Flight Ctr, Code Mech Engn Branch 543, Greenbelt, MD 20770 USA.
RP Bruck, HA (reprint author), Aerosp Corp, Space Mat Lab, Dept Mat Sci, POB 92957,M2-242, Los Angeles, CA 90009 USA.
EM bruck@umd.edu
FU Innovative Partnerships Program (IPP) Office at Goddard Space Flight
Center [N000140910640]; Aerospace Corporation's Independent Research and
Development Program (IRD)
FX The authors would like to acknowledge financial support from The
Innovative Partnerships Program (IPP) Office at Goddard Space Flight
Center, ONR award N000140910640, and The Aerospace Corporation's
Independent Research and Development Program (IR&D).
NR 18
TC 22
Z9 22
U1 0
U2 15
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 JUN
PY 2010
VL 41
IS 6
BP 729
EP 736
DI 10.1016/j.compositesa.2010.02.002
PG 8
WC Engineering, Manufacturing; Materials Science, Composites
SC Engineering; Materials Science
GA 593XK
UT WOS:000277496100004
ER
PT J
AU Fletcher, A
Gupta, MC
Dudley, KL
Vedeler, E
AF Fletcher, Alan
Gupta, Mool C.
Dudley, Kenneth L.
Vedeler, Erik
TI Elastomer foam nanocomposites for electromagnetic dissipation and
shielding applications
SO COMPOSITES SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Carbon nanotubes; Polymers; Nano composites; Electrical properties
ID POLYMER COMPOSITES; CARBON NANOTUBE; NANOFIBER
AB A novel elastomer foamed nanocomposite has been developed with high electromagnetic dissipation and shielding properties. This light weight foamed fluorocarbon incorporates multi-walled carbon nanotubes at low loading concentrations to achieve levels of conductivity and energy shielding that surpass the requirements for electromagnetic static discharge (ESD) and electromagnetic interference (EMI) shielding. Foaming the elastomer reduces that weight by 30% with minimal impact on ESD or EMI characteristics. The percolation threshold is at about 2% carbon nanotubes and the saturation conductivity occurs at 8% carbon nanotubes by weight. Combining the good electrical properties with the flexibility and fluid resistance of fluorocarbon yields a very versatile yet light weight material for a variety of ESD and EMI applications. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Fletcher, Alan] Univ Virginia, Dept Mat Sci & Engn, Charlottesville, VA 22904 USA.
[Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Dudley, Kenneth L.; Vedeler, Erik] NASA, Langley Res Ctr, Electromagnet Res Branch, Hampton, VA 23681 USA.
RP Gupta, MC (reprint author), 351 McCormick Rd,POB 400743, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
FU NASA Langley
FX Starting material and technical consulting was obtained from Hyperion
Catalysis International. Fluorocarbon compounding advise was kindly
provided by Eric Thomas formerly of DuPont Performance Elastomers and
Allen Sohlo of Dyneon Corp. EMI shielding and nanocomposite information
was provided by Max Alexander of the Air Force Research Laboratory. We
also thank NASA Langley for their Langley Professor program support.
NR 11
TC 65
Z9 67
U1 6
U2 48
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0266-3538
J9 COMPOS SCI TECHNOL
JI Compos. Sci. Technol.
PD JUN
PY 2010
VL 70
IS 6
BP 953
EP 958
DI 10.1016/j.compscitech.2010.02.011
PG 6
WC Materials Science, Composites
SC Materials Science
GA 595TE
UT WOS:000277635200010
ER
PT J
AU Beghin, C
Sotin, C
Hamelin, M
AF Beghin, Christian
Sotin, Christophe
Hamelin, Michel
TI Titan's native ocean revealed beneath some 45 km of ice by a
Schumann-like resonance
SO COMPTES RENDUS GEOSCIENCE
LA English
DT Article
DE Titan; Atmospheres; Ionospheres; Magnetospheres; Planet interiors
ID HUYGENS PROBE; ELECTRICAL-CONDUCTIVITY; DIELECTRIC-PROPERTIES;
AMMONIUM-SULFATE; ATMOSPHERE; DESCENT; SURFACE; MODEL; SATELLITES;
CALLISTO
AB After five years of thorough analysis of data from the Huygens Probe that descended into Titan's atmosphere in January 2005, we report major findings inferred from measurements of low frequency waves and atmospheric conductivity. The data account for the observation of a Schumann-like resonance trapped within Titan's atmospheric cavity. On Earth, this phenomenon is triggered by lightning and was anticipated to be observed on Titan, as it provides a tool to reveal the presence of a ground conductive boundary to sustain the resonance of the cavity. The Huygens observations show that the major electric field component of the signal is horizontal, which is inconsistent with lightning sources. We interpret, however, the observed signal as a second spherical harmonic of Titan's cavity, triggered and sustained by strong electric currents induced in the ionosphere by Saturn's magnetospheric plasma flow. The present study describes the characteristics of such trapped modes that allow us to constrain the parameters of the cavity and to infer the presence of a conductive layer at 45 km (+/- 15 km) below the surface. By comparison with the presence of subsurface conductive ocean in the Galilean icy satellites, we conclude that Titan should have pursued similar processes of internal dynamics. To date, this result represents the only evidence for a buried ocean in Titan. (C) 2010 Academie des sciences. Published by Elsevier Masson SAS. All rights reserved.
C1 [Beghin, Christian] Univ Orleans, CNRS, Lab Phys & Chim Espace & Environm, F-45071 Orleans, France.
[Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hamelin, Michel] Univ Versailles St Quentin, IPSL, LATMOS, F-94107 St Maur, France.
RP Beghin, C (reprint author), Univ Orleans, CNRS, Lab Phys & Chim Espace & Environm, 3A Ave Rech Sci, F-45071 Orleans, France.
EM cbeghin@cnrs-orleans.fr
NR 47
TC 21
Z9 21
U1 0
U2 4
PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75724 PARIS, FRANCE
SN 1631-0713
J9 CR GEOSCI
JI C. R. Geosci.
PD JUN
PY 2010
VL 342
IS 6
BP 425
EP 433
DI 10.1016/j.crte.2010.03.003
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA 626RD
UT WOS:000279983700001
ER
PT J
AU Bare, AY
Grimshaw, KL
Rooney, JJ
Sabater, MG
Fenner, D
Carroll, B
AF Bare, A. Y.
Grimshaw, K. L.
Rooney, J. J.
Sabater, M. G.
Fenner, D.
Carroll, B.
TI Mesophotic communities of the insular shelf at Tutuila, American Samoa
SO CORAL REEFS
LA English
DT Article
DE Mesophotic coral ecosystem; Insular shelf; Submerged banks; Coral reefs;
Tutuila; American Samoa
ID SCLERACTINIAN CORALS; REEF; DEEP; ZONATION
AB An investigation into the insular shelf and submerged banks surrounding Tutuila, American Samoa, was conducted using a towed camera system. Surveys confirmed the presence of zooxanthellate scleractinian coral communities at mesophotic depths (30-110 m). Quantification of video data, separated into 10-m-depth intervals, yielded a vertical, landward-to-seaward and horizontal distribution of benthic assemblages. Hard substrata composed a majority of bottom cover in shallow water, whereas unconsolidated sediments dominated the deep insular shelf and outer reef slopes. Scleractinian coral cover was highest atop mid-shelf patch reefs and on the submerged bank tops in depths of 30-50 m. Macroalgal cover was highest near shore and on reef slopes approaching the bank tops at 50-60 m. Percent cover of scleractinian coral colony morphology revealed a number of trends. Encrusting corals belonging to the genus Montipora were most abundant at shallow depths with cover gradually decreasing as depth increased. Massive corals, such as Porites spp., displayed a similar trend. Percent cover values of plate-like corals formed a normal distribution, with the highest cover observed in the 60-70 m depth range. Shallow plate-like corals belonged mostly to the genus Acropora and appeared to be significantly prevalent on the northeastern and eastern banks. Deeper plate-like corals on the reef slopes were dominated by Leptoseris, Pachyseris, or Montipora genera. Branching coral cover was high in the 80-110 m depth range. Columnar and free-living corals were also occasionally observed from 40-70 m.
C1 [Bare, A. Y.; Grimshaw, K. L.; Rooney, J. J.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv,Kewalo Res Facil, Honolulu, HI 96814 USA.
[Sabater, M. G.; Fenner, D.; Carroll, B.] Amer Samoa Dept Marine & Wildlife Resources, Pago Pago, AS 96799 USA.
RP Bare, AY (reprint author), Univ Hawaii, Joint Inst Marine & Atmospher Res, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv,Kewalo Res Facil, 1125-B Ala Moana Blvd, Honolulu, HI 96814 USA.
EM abare@hawaii.edu; John.Rooney@noaa.gov
FU NOAA
FX Funding to the NOAA Pacific Islands Fisheries Science Center's Coral
Reef Ecosystem Division for scientific expeditions to American Samoa was
provided by the NOAA Coral Reef Conservation Program. We greatly
appreciate the field assistance of Emily Hirsch, Frances Lichowski, and
Gillian Clague. We also express our gratitude to Kurt Hagedorn and Andy
Wearing of the M/V Bonavista II.
NR 21
TC 20
Z9 20
U1 2
U2 12
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
J9 CORAL REEFS
JI Coral Reefs
PD JUN
PY 2010
VL 29
IS 2
BP 369
EP 377
DI 10.1007/s00338-010-0600-y
PG 9
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 592WJ
UT WOS:000277412000010
ER
PT J
AU Samanta, A
Anderson, BT
Ganguly, S
Knyazikhin, Y
Nemani, RR
Myneni, RB
AF Samanta, Arindam
Anderson, Bruce T.
Ganguly, Sangram
Knyazikhin, Yuri
Nemani, Ramakrishna R.
Myneni, Ranga B.
TI EARTH Interactions
SO EARTH INTERACTIONS
LA English
DT Article
DE Forcing; Feedback; Climate
ID STRATOSPHERIC WATER-VAPOR; BREWER-DOBSON CIRCULATION; CLIMATE-CHANGE;
GREENHOUSE GASES; ALBEDO FEEDBACK; OVERSHOOT; SENSITIVITY; FORCINGS;
SYSTEM; WELL
AB Recent research indicates that the warming of the climate system resulting from increased greenhouse gas (GHG) emissions over the next century will persist for many centuries after the cessation of these emissions, principally because of the persistence of elevated atmospheric carbon dioxide (CO(2)) concentrations and their attendant radiative forcing. However, it is unknownwhether the responses of other components of the climate system-including those related to Greenland and Antarctic ice cover, the Atlantic thermohaline circulation, the West African monsoon, and ecosystem and human welfare would be reversed even if atmospheric CO(2) concentrations were to recover to 1990 levels. Here, using a simple set of experiments employing a current-generation numerical climate model, the authors examine the response of the physical climate system to decreasing CO(2) concentrations following an initial increase. Results indicate that many characteristics of the climate system, including global temperatures, precipitation, soil moisture, and sea ice, recover as CO(2) concentrations decrease. However, other components of the Earth system may still exhibit nonlinear hysteresis. In these experiments, for instance, increases in stratospheric water vapor, which initially result from increased CO(2) concentrations, remain present even as CO(2) concentrations recover. These results suggest that identification of additional threshold behaviors in response to human-induced global climate change should focus on subcomponents of the full Earth system, including cryosphere, biosphere, and chemistry.
C1 [Samanta, Arindam] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Ganguly, Sangram] NASA, Ames Res Ctr, BAERI, Moffett Field, CA 94035 USA.
RP Samanta, A (reprint author), Boston Univ, Dept Geog & Environm, 675 Commonwealth Ave, Boston, MA 02215 USA.
EM arindam.sam@gmail.com
RI Samanta, Arindam/B-9550-2009; ganguly, sangram/B-5108-2010; Myneni,
Ranga/F-5129-2012
FU NASA AMES Research Center; Boston University; National Center for
Atmospheric Research
FX We acknowledge support from A. Michaelis (NASA AMES Research Center), M.
Dugan (Boston University), and R. Neale (National Center for Atmospheric
Research).
NR 37
TC 1
Z9 1
U1 1
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1087-3562
J9 EARTH INTERACT
JI Earth Interact.
PD JUN
PY 2010
VL 14
AR 7
DI 10.1175/2010EI325.1
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA 614QQ
UT WOS:000279075200001
ER
PT J
AU Narock, T
Cragin, M
AF Narock, Tom
Cragin, Melissa
TI Earth and space science informatics infrastructure
SO EARTH SCIENCE INFORMATICS
LA English
DT Editorial Material
ID DESIGN
C1 [Narock, Tom] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA.
[Cragin, Melissa] Univ Illinois, Grad Sch Lib & Informat Sci, Urbana, IL USA.
RP Narock, T (reprint author), Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD USA.
EM Thomas.W.Narock@nasa.gov
OI Narock, Tom/0000-0002-9785-4496
NR 12
TC 0
Z9 0
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 1
EP 3
DI 10.1007/s12145-009-0041-8
PG 3
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100001
ER
PT J
AU Worrilow, K
King, T
Walker, R
Rose, ME
Moore, W
Joy, S
AF Worrilow, Kica
King, Todd
Walker, Raymond
Rose, Mark E.
Moore, William
Joy, Steven
TI Designing science web sites
SO EARTH SCIENCE INFORMATICS
LA English
DT Article; Proceedings Paper
CT ESSI Workshop
CY AUG 03-05, 2009
CL Baltimore, MD
SP ESSI
DE Website; Design; Science; Process
AB From a scientist's viewpoint a web site is one tool used to conduct research. From an artist's viewpoint web sites are a form of visual composition. From a developer's point of view a web site is a type of application. While web sites are a relatively new medium with a particular set of constraints, they do adhere to the same basic design principles that apply to other art forms. These design principles are the basic assumptions that affect the arrangement of elements within a composition. A successful design uses the principles and elements to achieve a visual goal in the composition. A web site designed for scientists has unique properties which are not shared by many other types of web sites. These properties influence the overall visual design of the web sites. Recently at the Institute of Geophysics and Planetary Physics at UCLA undertook a re-design of a number of its websites. In the effort, the use of visual design principles combined with the properties of a science web site were put to the test. In all, six different web sites were designed each with a difference science focus. We describe the process used to design the web sites which involve forming teams of designers, scientists and developers. We present example pages from each design and conclude with a discussion of what was learned during the process.
C1 [King, Todd; Walker, Raymond; Moore, William; Joy, Steven] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Worrilow, Kica] Kica Design, Marina Del Rey, CA 90292 USA.
[Rose, Mark E.] NASA, Ames Res Ctr, Perot Syst Govt Serv Inc PSGS, Moffett Field, CA 94035 USA.
RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM tking@igpp.ucla.edu
NR 6
TC 0
Z9 0
U1 0
U2 5
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 51
EP 57
DI 10.1007/s12145-010-0058-z
PG 7
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100006
ER
PT J
AU Tilmes, C
Yesha, Y
Halem, M
AF Tilmes, Curt
Yesha, Yelena
Halem, Milton
TI Tracking provenance of earth science data
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Data processing; Provenance
AB Tremendous volumes of data have been captured, archived and analyzed. Sensors, algorithms and processing systems for transforming and analyzing the data are evolving over time. Web Portals and Services can create transient data sets on-demand. Data are transferred from organization to organization with additional transformations at every stage. Provenance in this context refers to the source of data and a record of the process that led to its current state. It encompasses the documentation of a variety of artifacts related to particular data. Provenance is important for understanding and using scientific datasets, and critical for independent confirmation of scientific results. Managing provenance throughout scientific data processing has gained interest lately and there are a variety of approaches. Large scale scientific datasets consisting of thousands to millions of individual data files and processes offer particular challenges. This paper uses the analogy of art history provenance to explore some of the concerns of applying provenance tracking to earth science data. It also illustrates some of the provenance issues with examples drawn from the Ozone Monitoring Instrument (OMI) Data Processing System (OMIDAPS) (Tilmes et al. 2004) run at NASA's Goddard Space Flight Center by the first author.
C1 [Tilmes, Curt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yesha, Yelena; Halem, Milton] Univ Maryland, Baltimore, MD 21250 USA.
RP Tilmes, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Curt.Tilmes@nasa.gov; yeyesha@umbc.edu; halem@umbc.edu
RI Tilmes, Curt/D-5637-2012;
OI Tilmes, Curt/0000-0002-6512-0287
NR 11
TC 10
Z9 11
U1 1
U2 7
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 59
EP 65
DI 10.1007/s12145-010-0046-3
PG 7
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100007
ER
PT J
AU King, T
Thieman, J
Roberts, DA
AF King, Todd
Thieman, James
Roberts, D. Aaron
TI SPASE 2.0: a standard data model for space physics
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE SPASE; Data model; Ontology; Vocabulary; Heliophysics; Space physics;
Standard
AB SPASE-for Space Physics Archive Search and Extract-is a group with a charter to promote collaboration and sharing of data for the Space Plasma Physics community. A major activity is the definition of the SPASE Data Model which defines the metadata necessary to describe resources in the broader heliophysics data environment. The SPASE Data Model is primarily a controlled vocabulary with hierarchical relationships and with the ability to form associations between described resources. It is the result of many years of effort by an international collaboration (see http://www.spase-group.org) to unify and improve on existing Space and Solar Physics data models. The genesis of the SPASE group can be traced to 1998 when a small group of individuals saw a need for a data model. Today SPASE has a large international participation from many of the major space research organizations. The design of the data model is based on a set of principles derived from evaluation of the existing heliophysics data environment. The development guidelines for the data model are consistent with ISO-2788 (expanded in ANSI/NISO Z39.19) and the administration for the data model is comparable to that described in the ISO standards ISO-11179 and ISO-20943. Since the release of version 1.0 of the data model in 2005, the model has undergone a series of evolutions. SPASE released version 2.0 of its data model in April 2009. This version presents a significant change from the previous release. It includes the capability to describe a wider range of data products and to describe expert annotations which can be associated with a resource. Additional improvements include an enhanced capability to describe resource associations and a more unified approach to describing data products. Version 2.0 of the SPASE Data Model provides a solid foundation for continued integration of worldwide research activities and the open sharing of data.
C1 [King, Todd] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Thieman, James; Roberts, D. Aaron] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
EM tking@igpp.ucla.edu; james.r.thieman@nasa.gov; aaron.roberts@nasa.gov
FU National Aeronautics and Space Administration [NNX09AF15G]
FX This work was supported in part by the National Aeronautics and Space
Administration under Grant No. NNX09AF15G.
NR 12
TC 4
Z9 5
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 67
EP 73
DI 10.1007/s12145-010-0053-4
PG 7
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100008
ER
PT J
AU Marshall, JJ
Downs, RR
Samadi, S
AF Marshall, James J.
Downs, Robert R.
Samadi, Shahin
TI Relevance of software reuse in building advanced scientific data
processing systems
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Reuse; Data systems; Earth science; Software development; Software
adoption
AB Reuse of software and related components can contribute to the development of systems for processing scientific data. The reuse of components, which can be from any stage of the development life cycle, provides opportunities to realize benefits such as reduced costs and learning curves. However, the reuse of existing components also comes with risks that must be recognized in order to be mitigated. The National Aeronautics and Space Administration established the Earth Science Data Systems Software Reuse Working Group to support software reuse among members of the community of Earth science data systems developers. This is done through a variety of activities, including research, education, and public out-reach, which are conducted to help encourage and enable reuse within the community. Considerations for realizing the benefits of software reuse and minimizing risks are presented along with recent working group activities to improve reuse capabilities for the community of Earth science data systems developers.
C1 [Marshall, James J.] NASA, Goddard Space Flight Ctr, INNOVIM NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Downs, Robert R.] Columbia Univ, CIESIN, Palisades, NY 10964 USA.
[Samadi, Shahin] INNOVIM, INNOVIM NASA Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
RP Marshall, JJ (reprint author), NASA, Goddard Space Flight Ctr, INNOVIM NASA Goddard Space Flight Ctr, Mailstop 614-9, Greenbelt, MD 20771 USA.
EM James.J.Marshall@nasa.gov; rdowns@ciesin.columbia.edu;
Shahin.Samadi@nasa.gov
RI Marshall, James/A-9611-2009; Downs, Robert/B-4153-2013
OI Marshall, James/0000-0002-6867-5616; Downs, Robert/0000-0002-8595-5134
FU National Aeronautics and Space Administration [NNG08HZ11C]
FX The authors are grateful to the members of the National Aeronautics and
Space Administration (NASA) Earth Science Data Systems Software Reuse
Working Group who have contributed to the efforts described in this
paper, to the anonymous reviewers of earlier drafts who kindly offered
suggestions for improving the paper, and to Chris A. Mattmann and Neal
Most who offered valuable suggestions for improving earlier drafts of
the paper. The authors also appreciate the support for this work that
has been received from the National Aeronautics and Space
Administration, especially support received for Robert Downs under
contract NNG08HZ11C.
NR 24
TC 2
Z9 2
U1 1
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 95
EP 100
DI 10.1007/s12145-010-0054-3
PG 6
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100011
ER
PT J
AU Boller, RA
Braun, SA
Miles, J
Laidlaw, DH
AF Boller, Ryan A.
Braun, Scott A.
Miles, Jadrian
Laidlaw, David H.
TI Application of uncertainty visualization methods to meteorological
trajectories
SO EARTH SCIENCE INFORMATICS
LA English
DT Article
DE Uncertainty visualization; Multi-field visualization; Flow
visualization; Time-varying data; Meteorological visualization
techniques
ID VECTOR-FIELDS; MODEL; RESOLUTION; ACCURACY; ERRORS
AB We present an application of uncertainty visualization to air parcel trajectories generated from a global meteorological model. We derive an approximation of advection uncertainty due to interpolation and incorporate this uncertainty into our visualization of trajectories. Our work enables efficient visual pruning of unlikely results, especially in regions of atmospheric shear, potentially reducing erroneous interpretations. Finally, we apply these methods to a real-world meteorological problem to demonstrate its use.
C1 [Boller, Ryan A.; Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Miles, Jadrian; Laidlaw, David H.] Brown Univ, Dept Comp Sci, Providence, RI 02912 USA.
RP Boller, RA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM Ryan.A.Boller@nasa.gov
FU Software Engineering Division at NASA/Goddard Space Flight Center
FX The authors wish to thank E.J. Kalafarski/Brown University for
implementation of the Runge-Kutta integration algorithm along with Jim
Byrnes and the Software Engineering Division at NASA/Goddard Space
Flight Center for their support of this research.
NR 21
TC 2
Z9 2
U1 0
U2 2
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 119
EP 126
DI 10.1007/s12145-010-0052-5
PG 8
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100014
ER
PT J
AU King, T
Merka, J
Narock, T
Walker, R
Bargatze, L
AF King, Todd
Merka, Jan
Narock, Thomas
Walker, Raymond
Bargatze, Lee
TI A registry framework and Rosetta attributes for distributed science
SO EARTH SCIENCE INFORMATICS
LA English
DT Article; Proceedings Paper
CT ESSI Workshop
CY AUG 03-05, 2009
CL Baltimore, MD
SP ESSI
DE Data model; Framework; Registry; SPASE; Task oriented registry; Virtual
observatory
AB Information is shared within organizations and between organizations at an ever increasing rate. One system design that enables sharing in a distributed environment is a Virtual Observatory. A Virtual Observatory is built with clearly specified and standardized components. One essential component is a data model for the exchange of metadata. Well designed data models are compatible with the tenets of the ISO-11179 and ISO-20943 standards for metadata registries. Another essential component is the specification for persistent universal identifiers which are used to reference resources provided through the system. Identifiers are used both to link harvested information back to the original resource description and by services to retrieve a resource. Harvested information is maintained in a registry. To harvest information from a set of metadata it is necessary to understand the schema of the metadata. We propose an approach to the formation of universal identifiers which enables one to clearly discern the schema of the source metadata. A primary registry containing a broad set of base information exists in every Virtual Observatory. Specialized Task Oriented Registries (TOR) are typically derived from the primary registry. The schema in a TOR is often flat and items in the TOR can be managed in a similar manner to that prescribed in ISO-11179. The need for interoperability within a data environment and between data environments leads to the identification of broad-based, common attributes we call "Rosetta Attributes" which will enable general cross domain searches. Access to metadata is the final component of a Virtual Observatory. Access is provided by a registry service. A specification for a minimal registry service is presented.
C1 [King, Todd; Walker, Raymond; Bargatze, Lee] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Walker, Raymond] Univ Calif Los Angeles, Earth & Space Sci Dept, Los Angeles, CA 90095 USA.
[Merka, Jan; Narock, Thomas] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20771 USA.
[Merka, Jan; Narock, Thomas] Univ Maryland, Baltimore, MD 21250 USA.
RP King, T (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM tking@igpp.ucla.edu
OI Narock, Tom/0000-0002-9785-4496
NR 15
TC 0
Z9 0
U1 1
U2 1
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1865-0473
J9 EARTH SCI INFORM
JI Earth Sci. Inform.
PD JUN
PY 2010
VL 3
IS 1-2
BP 127
EP 133
DI 10.1007/s12145-010-0047-2
PG 7
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 703XH
UT WOS:000286014100015
ER
PT J
AU Bignell, J
LaFave, J
AF Bignell, John
LaFave, James
TI Analytical fragility analysis of southern Illinois wall pier supported
highway bridges
SO EARTHQUAKE ENGINEERING & STRUCTURAL DYNAMICS
LA English
DT Article
DE fragility analysis; wall pier; bridge; earthquake; liquefaction; New
Madrid Seismic Zone
ID LIQUEFACTION RESISTANCE; INTENSITY
AB An analytical fragility analysis was conducted in order to characterize the seismic vulnerability of existing southern Illinois wall pier supported highway bridges to potential earthquakes. To perform this fragility analysis, a detailed inventory survey was first taken of the wall pier bridges identified in an earlier random sampling of southern Illinois priority emergency route bridges. From the survey three types of wall pier bridges were identified. Of those identified, hammerhead and regular wall pier supported bridges represented nearly 90% of the population. Incorporating structural variations determined from the random sample survey, nearly 100 three-dimensional nonlinear finite element models were constructed. Each model was subjected to a randomly assigned synthetic earthquake representative of those that could potentially occur within the region. From these analyses, a series of wall pier supported bridge fragility curves were produced. In addition, a liquefaction fragility analysis was conducted in order to characterize the seismic vulnerability of southern Illinois wall pier supported highway bridge sites to liquefaction in potential earthquakes. To perform this second fragility analysis, wall pier bridges within the southern Illinois random sample that may be susceptible to liquefaction were identified. A soil profile from each of these susceptible bridge sites was then subjected to randomly assigned bedrock motions, and an Arias intensity liquefaction analysis was carried out. From these analyses, a fragility curve for the potentially liquefiable wall pier supported bridge sites was produced. Overall results of this study indicate that southern Illinois wall pier supported bridges are moderately vulnerable to structural damage in a 2% probability of exceedance in 50 year earthquake, and in some cases they could also be highly vulnerable to on-site liquefaction events. Copyright (C) 2009 John Wiley & Sons, Ltd.
C1 [Bignell, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[LaFave, James] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
RP Bignell, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 303-410, Pasadena, CA 91109 USA.
EM jlbignell@gmail.com
FU Illinois Department of Transportation (IDOT) [IHR-R36]; National
Computational Science Alliance (NCSA) [BCS400001N]
FX Contract/grant sponsor: Illinois Department of Transportation (IDOT);
contract/grant number: IHR-R36; Contract/grant sponsor: National
Computational Science Alliance (NCSA); contract/grant number: BCS400001N
NR 40
TC 5
Z9 5
U1 0
U2 7
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 0098-8847
J9 EARTHQ ENG STRUCT D
JI Earthq. Eng. Struct. Dyn.
PD JUN
PY 2010
VL 39
IS 7
BP 709
EP 729
DI 10.1002/eqe.966
PG 21
WC Engineering, Civil; Engineering, Geological
SC Engineering
GA 591VC
UT WOS:000277332100001
ER
PT J
AU van Donkelaar, A
Martin, RV
Brauer, M
Kahn, R
Levy, R
Verduzco, C
Villeneuve, PJ
AF van Donkelaar, Aaron
Martin, Randall V.
Brauer, Michael
Kahn, Ralph
Levy, Robert
Verduzco, Carolyn
Villeneuve, Paul J.
TI Global Estimates of Ambient Fine Particulate Matter Concentrations from
Satellite-Based Aerosol Optical Depth: Development and Application
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
DE aerosol; aerosol optical depth; AOD; particulate matter; PM2.5
ID GROUND-LEVEL PM2.5; AIR-POLLUTION; UNITED-STATES; QUALITY; MORTALITY;
THICKNESS; MODIS; CITIES; COHORT
AB BACKGROUND: Epidemiologic and health impact studies of fine particulate matter with diameter < 2.5 mu m (PM2.5) are limited by the lack of monitoring data, especially in developing countries. Satellite observations offer valuable global information about PM2.5 concentrations.
OBJECTIVE: In this study, we developed a technique for estimating surface PM2.5 concentrations from satellite observations.
METHODS: We mapped global ground-level PM2.5 concentrations using total column aerosol optical depth (AOD) from the MODIS (Moderate Resolution Imaging Spectroradiometer) and MISR (Multiangle Imaging Spectroradiometer) satellite instruments and coincident aerosol vertical profiles from the GEOS-Chem global chemical transport model.
RESULTS: We determined that global estimates of long-term average (1 January 2001 to 31 December 2006) PM2.5 concentrations at approximately 10 km x 10 km resolution indicate a global population-weighted geometric mean PM2.5 concentration of 20 mu g/m(3). The World Health Organization Air Quality PM2.5 Interim Target-1 (35 mu g/m(3) annual average) is exceeded over central and eastern Asia for 38% and for 50% of the population, respectively. Annual mean PM2.5 concentrations exceed 80 mu g/m(3) over eastern China. Our evaluation of the satellite-derived estimate with ground-based in situ measurements indicates significant spatial agreement with North American measurements (r = 0.77; slope = 1.07; n = 1057) and with noncoincident measurements elsewhere (r = 0133; slope = 0.86; n = 244). The 1 SD of uncertainty in the satellite-derived PM2.5 is 25%, which is inferred from the AOD retrieval and from aerosol vertical profile errors and sampling. The global population-weighted mean uncertainty is 6.7 mu g/m(3).
CONCLUSIONS: Satellite-derived total-column AOD, when combined with a chemical transport model, provides estimates of global long-term average PM2.5 concentrations.
C1 [van Donkelaar, Aaron; Martin, Randall V.; Verduzco, Carolyn] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brauer, Michael] Univ British Columbia, Sch Environm Hlth, Vancouver, BC V5Z 1M9, Canada.
[Kahn, Ralph; Levy, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Villeneuve, Paul J.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada.
[Villeneuve, Paul J.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada.
RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada.
EM Aaron.van.Donkelaar@dal.ca
RI Levy, Robert/M-7764-2013; Martin, Randall/C-1205-2014; Kahn,
Ralph/D-5371-2012; Chem, GEOS/C-5595-2014;
OI Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402;
Kahn, Ralph/0000-0002-5234-6359; Brauer, Michael/0000-0002-9103-9343
FU Health Canada [4500171909, 4500220294]; Natural Sciences and Engineering
Research of Canada; Killam Trust
FX This study was funded by contracts from Health Canada (4500171909 and
4500220294). A.v.D. was supported by graduate fellowships from the
Natural Sciences and Engineering Research of Canada and the Killam
Trust.
NR 45
TC 398
Z9 402
U1 43
U2 301
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
EI 1552-9924
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD JUN
PY 2010
VL 118
IS 6
BP 847
EP 855
DI 10.1289/ehp.0901623
PG 9
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 608NP
UT WOS:000278591300031
PM 20519161
ER
PT J
AU Kharecha, PA
Kutscher, CF
Hansen, JE
Mazria, E
AF Kharecha, Pushker A.
Kutscher, Charles F.
Hansen, James E.
Mazria, Edward
TI Options for Near-Term Phaseout of CO2 Emissions from Coal Use in the
United States
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Review
ID LIFE-CYCLE; ELECTRICITY-GENERATION; ENERGY EFFICIENCY; POWER-GENERATION;
CARBON CAPTURE; NUCLEAR-POWER; BIOMASS; SYSTEMS; STORAGE; DESIGN
AB The global climate problem becomes tractable if CO2 emissions from coal use are phased out rapidly and emissions from unconventional fossil fuels (e.g., oil shale and tar sands) are prohibited. This paper outlines technology options for phasing out coal emissions in the United States by similar to 2030. We focus on coal for physical and practical reasons and on the U.S. because it is most responsible for accumulated fossil fuel CO2 in the atmosphere today, specifically targeting electricity production, which is the primary use of coal. While we recognize that coal emissions must be phased out globally, we believe U.S. leadership is essential, A major challenge for reducing U.S. emissions is that coal provides the largest proportion of base load power, i.e., power satisfying minimum electricity demand. Because this demand is relatively constant and coal has a high carbon intensity, utility carbon emissions are largely due to coal. The current U.S. electric grid incorporates little renewable power, most of which is not base load power. However, this can readily be changed within the next 2-3 decades. Eliminating coal emissions also requires improved efficiency, a "smart grid", additional energy storage, and advanced nuclear power. Any further coal usage must be accompanied by carbon capture and storage (CCS). We suggest that near-term emphasis should be on efficiency measures and substitution of coal-fired power by renewables and third-generation nuclear plants, since these technologies have been successfully demonstrated at the relevant (commercial) scale. Beyond 2030, these measures can be supplemented by CCS at power plants and, as needed, successfully demonstrated fourth-generation reactors. We conclude that U.S. coal emissions could be phased out by 2030 using existing technologies or ones that could be commercially competitive with coal within about a decade. Elimination of fossil fuel subsidies and a substantial rising price on carbon emissions are the root requirements for a clean, emissions-free future.
C1 [Kharecha, Pushker A.; Hansen, James E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Kharecha, Pushker A.; Hansen, James E.] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Kutscher, Charles F.] Natl Renewable Energy Lab, Golden, CO 80401 USA.
[Mazria, Edward] 2030 Inc Architecture 2030, Santa Fe, NM 87505 USA.
RP Kharecha, PA (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM pushker@giss.nasa.gov
FU Lenfest Foundation
FX This paper was motivated by, and is based in part on, a workshop on
energy use and climate change mitigation held on Nov. 3, 2008 in
Washington, DC. The workshop was funded by the Lenfest Foundation, and
the presentations as well as participant biographies are archived at
www.mediafire.com/nov3workshop. The views in this paper are solely those
of the authors and do not necessarily represent the views of their
institutions or the other workshop participants. We are grateful to all
of the workshop participants and to Maggie Betancourt and Evelyn
DeJesus-Quiles for helping to coordinate the logistics. Colleagues at
NREL and Architecture 2030 were very helpful in providing figure data,
references, and comments. We also thank Revis James, Anelia Milbrandt,
Kathy O'Dell, Jeff Tester, Colin Williams, and Elsevier Publishing for
granting permission to reproduce figures, and three anonymous reviewers
for providing constructive comments on the draft manuscript.
NR 92
TC 13
Z9 13
U1 1
U2 39
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 JUN 1
PY 2010
VL 44
IS 11
BP 4050
EP 4062
DI 10.1021/es903884a
PG 13
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 600RA
UT WOS:000278003500007
PM 20429611
ER
PT J
AU Mijajlovic, M
Biggs, MJ
Djurdjevic, DP
AF Mijajlovic, Milan
Biggs, Mark J.
Djurdjevic, Dusan P.
TI On Potential Energy Models for EA-based Ab Initio Protein Structure
Prediction
SO EVOLUTIONARY COMPUTATION
LA English
DT Article
DE Biochemistry; biomaterials; biomedical engineering; bionanotechnology;
EA adaptivity; nanotechnology; surface binding proteins
ID DETERMINISTIC GLOBAL OPTIMIZATION; HYDROGEN-BOND INTERACTIONS; OCCURRING
AMINO-ACIDS; ATOM FORCE-FIELD; GENETIC ALGORITHM; MET-ENKEPHALIN;
NONBONDED INTERACTIONS; MOLECULAR-MECHANICS; EVOLUTIONARY ALGORITHMS;
GEOMETRICAL PARAMETERS
AB Ab initio protein structure prediction involves determination of the three-dimensional (3D) conformation of proteins on the basis of their amino acid sequence, a potential energy (PE) model that captures the physics of the interatomic interactions, and a method to search for and identify the global minimum in the PE (or free energy) surface such as an evolutionary algorithm (EA). Many PE models have been proposed over the past three decades and more. There is currently no understanding of how the behavior of an EA is affected by the PE model used. The study reported here shows that the EA behavior can be profoundly affected: the EA performance obtained when using the ECEPP PE model is significantly worse than that obtained when using the Amber, OPLS, and CVFF PE models, and the optimal EA control parameter values for the ECEPP model also differ significantly from those associated with the other models.
C1 [Mijajlovic, Milan] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Biggs, Mark J.] Univ Adelaide, Sch Chem Engn, Adelaide, SA 5005, Australia.
[Djurdjevic, Dusan P.] P&G Tech Ctr Ltd, Newcastle Upon Tyne, Tyne & Wear, England.
RP Mijajlovic, M (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Mail Stop 239-4, Moffett Field, CA 94035 USA.
EM mark.biggs@adelaide.edu.au
OI Biggs, Mark/0000-0002-2131-3677
FU University of Edinburgh; Overseas Research Support (ORS) Scheme; Royal
Academy of Engineering; Leverhulme Trust; eDIKT initiative
FX MM thanks the University of Edinburgh and Overseas Research Support
(ORS) Scheme for financial support. MJB thanks the Royal Academy of
Engineering and the Leverhulme Trust for the award of a RAEng/Leverhulme
Senior Research Fellowship. This work has made use of resources provided
by the Edinburgh Compute and Data Facility (www.ecdf.ed.ac.uk), which is
partially supported by the eDIKT initiative (www.edikt.org.uk).
NR 80
TC 3
Z9 3
U1 1
U2 5
PU M I T PRESS
PI CAMBRIDGE
PA 238 MAIN STREET, STE 500, CAMBRIDGE, MA 02142-1046 USA
SN 1063-6560
J9 EVOL COMPUT
JI Evol. Comput.
PD SUM
PY 2010
VL 18
IS 2
BP 255
EP 275
DI 10.1162/evco.2010.18.2.18204
PG 21
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods
SC Computer Science
GA 588VF
UT WOS:000277101800004
PM 20210597
ER
PT J
AU Ray, AE
Connon, SA
Sheridan, PP
Gilbreath, J
Shields, M
Newby, DT
Fujita, Y
Magnuson, TS
AF Ray, Allison E.
Connon, Stephanie A.
Sheridan, Peter P.
Gilbreath, Jeremy
Shields, Malcolm
Newby, Deborah T.
Fujita, Yoshiko
Magnuson, Timothy S.
TI Intragenomic heterogeneity of the 16S rRNA gene in strain UFO1 caused by
a 100-bp insertion in helix 6
SO FEMS MICROBIOLOGY ECOLOGY
LA English
DT Article
DE 16S rRNA genes; gene inserts; intragenomic heterogeneity; intervening
sequence (IVS); helix 6
ID NOV-SP NOV.; HALOARCULA-MARISMORTUI; INTERVENING SEQUENCES; COPY NUMBER;
BACTERIAL; OPERONS; SUBSURFACE; DIVERSITY; ENUMERATION; DIVERGENCE
AB Two different versions of the 16S rRNA gene, one of which contained an unusual 100-bp insertion in helix 6, were detected in isolate UFO1 acquired from the Oak Ridge Integrated Field-Research Challenge (ORIFRC) site in Tennessee. rRNA was extracted from UFO1 and analyzed by reverse transcriptase-quantitative PCR with insert- and non-insert-specific primers; only the noninsert 16S rRNA gene sequence was detected. Similarly, PCR-based screening of a cDNA library (190 clones) constructed from reverse-transcribed rRNA from UFO1 did not detect any clones containing the 100-bp insert. Examination of cDNA with primers specific to the insert-bearing 16S rRNA gene, but downstream of the insert, suggests that the insert was excised from rRNA. Inspection of other 16S rRNA genes in the GenBank database revealed that a homologous insert sequence, also found in helix 6, has been reported in other environmental clones, including those acquired from ORIFRC enrichments. These findings demonstrate the existence of widely divergent copies of the 16S rRNA gene within the same organism, which may confound 16S rRNA gene-based methods of estimating microbial diversity in environmental samples.
C1 [Ray, Allison E.; Newby, Deborah T.; Fujita, Yoshiko] Idaho Natl Lab, Biol Syst Dept, Idaho Falls, ID 83415 USA.
[Ray, Allison E.; Connon, Stephanie A.; Sheridan, Peter P.; Gilbreath, Jeremy; Shields, Malcolm; Magnuson, Timothy S.] Idaho State Univ, Dept Biol Sci, Pocatello, ID 83209 USA.
[Connon, Stephanie A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Ray, AE (reprint author), Idaho Natl Lab, Biol Syst Dept, POB 1625, Idaho Falls, ID 83415 USA.
EM alikona.ray@gmail.com
RI Connon, Stephanie/K-1959-2012; Fujita, Yoshiko/S-2007-2016
OI Fujita, Yoshiko/0000-0002-4472-4102
FU Idaho National Laboratory; Inland Northwest Research Alliance [ISU-004];
US Department of Energy [DE-FG02-04ER63626]
FX We would like to thank Hope Lee, Aren Eddingsaas, James Henriksen, Amber
Miller, Joni Barnes, Lynn Wendt, and Cindy Breckenridge for helpful
advice and technical assistance. We thank Erin O'Leary-Jepson and
Michelle Andrews of the Idaho State University Molecular Research Core
Facility for 16S rRNA gene sequencing. We also extend our thanks to
David Reed and Frank Roberto, of the INL for reviewing this manuscript
and providing helpful comments. This work was supported by the Idaho
National Laboratory, the Inland Northwest Research Alliance (Grant
Number ISU-004 to T. S. M., and Graduate Fellowship to A. E. R.), and
the US Department of Energy (Grant Number DE-FG02-04ER63626 to T. S.
M.).
NR 51
TC 7
Z9 7
U1 0
U2 8
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0168-6496
J9 FEMS MICROBIOL ECOL
JI FEMS Microbiol. Ecol.
PD JUN
PY 2010
VL 72
IS 3
BP 343
EP 353
DI 10.1111/j.1574-6941.2010.00868.x
PG 11
WC Microbiology
SC Microbiology
GA 591RR
UT WOS:000277321300003
PM 20557571
ER
PT J
AU Geng, T
Zheng, F
Kuznetsov, AV
Roberts, WL
Paxson, DE
AF Geng, Tao
Zheng, Fei
Kuznetsov, Andrey V.
Roberts, William L.
Paxson, Daniel E.
TI Comparison Between Numerically Simulated and Experimentally Measured
Flowfield Quantities Behind a Pulsejet
SO FLOW TURBULENCE AND COMBUSTION
LA English
DT Article
DE Pulsejet; Valve model; Exhaust flow field; Vortex location; Turbulence
ID VORTEX RING FORMATION; VALVELESS PULSEJET; TUBE; CIRCULATION; SCALE; JET
AB Pulsed combustion is receiving renewed interest as a potential route to higher performance in air breathing propulsion and ground based power generation systems. Pulsejets offer a simple experimental device with which to study unsteady combustion phenomena and validate simulations. Previous computational fluid dynamics (CFD) simulations focused primarily on pulsejet combustion and exhaust processes. This paper describes a new inlet sub-model which simulates the fluidic and mechanical operation of a valved pulsejet head. The governing equations for this sub-model are described. Sub-model validation is provided through comparisons of simulated and experimentally measured reed valve motion, and time averaged inlet mass flow rate. The updated pulsejet simulation, with the inlet sub-model implemented, is validated through comparison with experimentally measured combustion chamber pressure, inlet mass flow rate, operational frequency, and thrust. Additionally, the simulated pulsejet exhaust flowfield, which is dominated by a starting vortex ring, is compared with particle imaging velocimetry (PIV) measurements on the bases of velocity, vorticity, and vortex location. The results show good agreement between simulated and experimental data. The inlet sub-model is shown to be critical for the successful modeling of pulsejet operation. This sub-model correctly predicts both the inlet mass flow rate and its phase relationship with the combustion chamber pressure. As a result, the predicted pulsejet thrust agrees very well with experimental data.
C1 [Geng, Tao; Zheng, Fei; Kuznetsov, Andrey V.; Roberts, William L.] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA.
[Paxson, Daniel E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Kuznetsov, AV (reprint author), N Carolina State Univ, Dept Mech & Aerosp Engn, Campus Box 7910, Raleigh, NC 27695 USA.
EM avkuznet@eos.ncsu.edu
NR 27
TC 3
Z9 3
U1 4
U2 11
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 JUN
PY 2010
VL 84
IS 4
BP 653
EP 667
DI 10.1007/s10494-010-9247-6
PG 15
WC Thermodynamics; Mechanics
SC Thermodynamics; Mechanics
GA 606DT
UT WOS:000278402700006
ER
PT J
AU Xiong, XX
Cao, CY
Chander, G
AF Xiong, Xiaoxiong (Jack)
Cao, Changyong
Chander, Gyanesh
TI An overview of sensor calibration inter-comparison and applications
SO FRONTIERS OF EARTH SCIENCE
LA English
DT Review
DE radiometer; MODIS; AVHRR; ETM; calibration; inter-comparison
AB Long-term climate data records (CDR) are often constructed using observations made by multiple Earth observing sensors over a broad range of spectra and a large scale in both time and space. These sensors can be of the same or different types operated on the same or different platforms. They can be developed and built with different technologies and are likely operated over different time spans. It has been known that the uncertainty of climate models and data records depends not only on the calibration quality (accuracy and stability) of individual sensors, but also on their calibration consistency across instruments and platforms. Therefore, sensor calibration inter-comparison and validation have become increasingly demanding and will continue to play an important role for a better understanding of the science product quality. This paper provides an overview of different methodologies, which have been successfully applied for sensor calibration inter-comparison. Specific examples using different sensors, including MODIS, AVHRR, and ETM+, are presented to illustrate the implementation of these methodologies.
C1 [Xiong, Xiaoxiong (Jack)] NASA, GSFC, Sci Explorat Directorate, Greenbelt, MD 20771 USA.
[Cao, Changyong] NOAA, NESDIS, Off Res & Applicat, Camp Springs, MD 20746 USA.
[Chander, Gyanesh] US Geol Survey, SGT Inc, EROS Ctr, Sioux Falls, SD 57198 USA.
RP Xiong, XX (reprint author), NASA, GSFC, Sci Explorat Directorate, Greenbelt, MD 20771 USA.
EM Xiaoxiong.Xiong-1@nasa.gov
RI Cao, Changyong/F-5578-2010
NR 55
TC 7
Z9 7
U1 0
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 2095-0195
J9 FRONT EARTH SCI-PRC
JI Front. Earth Sci.
PD JUN
PY 2010
VL 4
IS 2
BP 237
EP 252
DI 10.1007/s11707-010-0002-z
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA V29CD
UT WOS:000208725600011
ER
PT J
AU Tangalos, GE
Beard, BL
Johnson, CM
Alpers, CN
Shelobolina, ES
Xu, H
Konishi, H
Roden, EE
AF Tangalos, G. E.
Beard, B. L.
Johnson, C. M.
Alpers, C. N.
Shelobolina, E. S.
Xu, H.
Konishi, H.
Roden, E. E.
TI Microbial production of isotopically light iron(II) in a modern
chemically precipitated sediment and implications for isotopic
variations in ancient rocks
SO GEOBIOLOGY
LA English
DT Article
ID FE(III) OXIDE REDUCTION; ACID-MINE WATERS; FE ISOTOPE; DISSIMILATORY
FE(III); WESTERN-AUSTRALIA; SULFATE REDUCTION; TRANSVAAL SUPERGROUP;
AQUATIC SEDIMENTS; MN(IV) REDUCTION; MARINE-SEDIMENTS
AB The inventories and Fe isotope composition of aqueous Fe(II) and solid-phase Fe compounds were quantified in neutral-pH, chemically precipitated sediments downstream of the Iron Mountain acid mine drainage site in northern California, USA. The sediments contain high concentrations of amorphous Fe(III) oxyhydroxides [Fe(III)(am)] that allow dissimilatory iron reduction (DIR) to predominate over Fe-S interactions in Fe redox transformation, as indicated by the very low abundance of Cr(II)-extractable reduced inorganic sulfur compared with dilute HCl-extractable Fe. delta 56Fe values for bulk HCl- and HF-extractable Fe were approximate to 0. These near-zero bulk delta 56Fe values, together with the very low abundance of dissolved Fe in the overlying water column, suggest that the pyrite Fe source had near-zero delta 56Fe values, and that complete oxidation of Fe(II) took place prior to deposition of the Fe(III) oxide-rich sediment. Sediment core analyses and incubation experiments demonstrated the production of millimolar quantities of isotopically light (delta 56Fe approximate to -1.5 to -0.5 parts per thousand) aqueous Fe(II) coupled to partial reduction of Fe(III)(am) by DIR. Trends in the Fe isotope composition of solid-associated Fe(II) and residual Fe(III)(am) are consistent with experiments with synthetic Fe(III) oxides, and collectively suggest an equilibrium Fe isotope fractionation between aqueous Fe(II) and Fe(III)(am) of approximately -2 parts per thousand. These Fe(III) oxide-rich sediments provide a model for early diagenetic processes that are likely to have taken place in Archean and Paleoproterozoic marine sediments that served as precursors for banded iron formations. Our results suggest pathways whereby DIR could have led to the formation of large quantities of low-delta 56Fe minerals during BIF genesis.
C1 [Tangalos, G. E.; Beard, B. L.; Johnson, C. M.; Shelobolina, E. S.; Xu, H.; Konishi, H.; Roden, E. E.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Tangalos, G. E.; Beard, B. L.; Johnson, C. M.; Shelobolina, E. S.; Xu, H.; Konishi, H.; Roden, E. E.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI USA.
[Alpers, C. N.] US Geol Survey, Calif Water Sci Ctr, Sacramento, CA USA.
RP Roden, EE (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
EM eroden@geology.wisc.edu
OI Alpers, Charles/0000-0001-6945-7365
FU NASA Astrobiology Institute; National Science Foundation [0525417]; US
Geological Survey
FX This research was funded by the NASA Astrobiology Institute (University
of California-Berkeley and University of Wisconsin-Madison nodes) and
the National Science Foundation (Biogeosciences Program Award 0525417).
Logistical support for field sampling was provided by the US Geological
Survey in cooperation with the US Environmental Protection Agency. We
thank Kurt Konhauser and three anonymous reviewers whose thoughtful
criticism substantially improved the manuscript.
NR 96
TC 23
Z9 26
U1 2
U2 30
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1472-4677
J9 GEOBIOLOGY
JI Geobiology
PD JUN
PY 2010
VL 8
IS 3
BP 197
EP 208
DI 10.1111/j.1472-4669.2010.00237.x
PG 12
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA 596NW
UT WOS:000277692900004
PM 20374296
ER
PT J
AU Berger, EL
Lauretta, DS
Zega, TJ
Keller, LP
AF Berger, E. L.
Lauretta, D. S.
Zega, T. J.
Keller, L. P.
TI Stardust and CI-chondrite sulfides
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Berger, E. L.; Lauretta, D. S.] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Zega, T. J.] USN, Res Lab, Washington, DC 20375 USA.
[Keller, L. P.] Johnson Space Ctr, Robert M Walker Lab Space Sci, ARES, Houston, TX 77573 USA.
EM elberger@lpl.arizona.edu
NR 2
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A81
EP A81
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401344
ER
PT J
AU Bodnarik, J
Evans, L
Floyd, S
Lim, L
Mcclanahan, T
Namkung, M
Parsons, A
Schweitzer, J
Starr, R
Trombka, J
AF Bodnarik, J.
Evans, L.
Floyd, S.
Lim, L.
Mcclanahan, T.
Namkung, M.
Parsons, A.
Schweitzer, J.
Starr, R.
Trombka, J.
TI In situ instrumentation for subsurface planetary geochemistry
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Bodnarik, J.; Evans, L.; Floyd, S.; Lim, L.; Mcclanahan, T.; Namkung, M.; Parsons, A.; Starr, R.; Trombka, J.] NASA GSFC, Greenbelt, MD 20771 USA.
[Schweitzer, J.] Univ Connecticut, Storrs, CT 06269 USA.
EM julia.g.bodnarik@nasa.gov
RI Lim, Lucy/C-9557-2012; Namkung, Min/E-1533-2012; Parsons,
Ann/I-6604-2012
OI Lim, Lucy/0000-0002-9696-9654;
NR 2
TC 0
Z9 0
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A100
EP A100
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401381
ER
PT J
AU Chabot, NL
McDonough, WF
Saslow, SA
Ash, RD
Draper, DS
Jones, JH
Agee, CB
AF Chabot, Nancy L.
McDonough, William F.
Saslow, Sarah A.
Ash, Richard D.
Draper, David S.
Jones, John H.
Agee, Carl B.
TI Partitioning behavior at pressure in the Fe-S System
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McDonough, William F.; Saslow, Sarah A.; Ash, Richard D.] Univ Maryland, College Pk, MD 20742 USA.
[Draper, David S.; Jones, John H.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Agee, Carl B.] Univ New Mexico, Albuquerque, NM 87131 USA.
EM Nancy.Chabot@JHUAPL.edu
RI Chabot, Nancy/F-5384-2015
OI Chabot, Nancy/0000-0001-8628-3176
NR 7
TC 0
Z9 0
U1 0
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A155
EP A155
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400559
ER
PT J
AU Czaja, AD
Johnson, CM
Beard, BL
Van Kranendonk, MJ
AF Czaja, Andrew D.
Johnson, Clark M.
Beard, Brian L.
Van Kranendonk, Martin J.
TI Iron isotopes reveal an abiological origin for a 2.75 Ga BIF from the
Yilgarn Craton, Western Australia
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Czaja, Andrew D.; Johnson, Clark M.; Beard, Brian L.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Czaja, Andrew D.; Johnson, Clark M.; Beard, Brian L.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
[Van Kranendonk, Martin J.] Dept Mines & Petr, Perth, WA 6009, Australia.
[Van Kranendonk, Martin J.] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia.
EM czaja@wisc.edu
RI Van Kranendonk, Martin/J-8755-2012
NR 0
TC 0
Z9 0
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A201
EP A201
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400652
ER
PT J
AU Flynn, GJ
Wirick, S
Keller, LP
Jacobsen, C
Sandford, SA
AF Flynn, G. J.
Wirick, S.
Keller, L. P.
Jacobsen, C.
Sandford, S. A.
TI Constraints on the formation mechanism of early Solar System organic
matter in primitive IDPs
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Flynn, G. J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA.
[Wirick, S.; Jacobsen, C.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Keller, L. P.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM george.Flynn@plattsburgh.edu
RI Jacobsen, Chris/E-2827-2015
OI Jacobsen, Chris/0000-0001-8562-0353
NR 3
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A298
EP A298
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400845
ER
PT J
AU Foustoukos, DI
Stern, JC
AF Foustoukos, D. I.
Stern, J. C.
TI Oxidation of organics under hydrothermal conditions: Implications for
the evolution of methane on Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Foustoukos, D. I.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
[Stern, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM dfoustoukos@ciw.edu; Jennifer.C.Stern@nasa.gov
RI Stern, Jennifer/E-3135-2012
OI Stern, Jennifer/0000-0002-0162-8807
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A302
EP A302
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400853
ER
PT J
AU Gleeson, D
Williamson, C
Wright, K
Spear, J
Pappalardo, R
Grasby, S
Templeton, A
AF Gleeson, Damnhait
Williamson, Chase
Wright, Katherine
Spear, John
Pappalardo, Robert
Grasby, Steve
Templeton, Alexis
TI Low temperature S biomineralization at a supraglacial spring system in
the Canadian High Arctic
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Gleeson, Damnhait; Wright, Katherine; Templeton, Alexis] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Williamson, Chase; Spear, John] Colorado Sch Mines, Golden, CO 80401 USA.
[Gleeson, Damnhait; Pappalardo, Robert] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Grasby, Steve] Geol Survey Canada, Calgary, AB T2L 2A7, Canada.
EM alexis.templeton@colorado.edu
NR 0
TC 0
Z9 0
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A338
EP A338
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401051
ER
PT J
AU Goldblatt, C
Zanhle, K
AF Goldblatt, Colin
Zanhle, Kevin
TI The subduction origin of mantle nitrogen
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Goldblatt, Colin; Zanhle, Kevin] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM colin.goldblatt@nasa.gov; kevin.j.zahnle@nasa.gov
NR 1
TC 0
Z9 0
U1 2
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 JUN
PY 2010
VL 74
IS 12
SU 1
BP A342
EP A342
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401059
ER
PT J
AU Hecht, MH
Kounaves, SP
AF Hecht, M. H.
Kounaves, S. P.
TI Aqueous chemistry on Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Kounaves, S. P.] Tufts Univ, Dept Chem, Medford, MA 02155 USA.
[Hecht, M. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM michael.h.hecht@jpl.nasa.gov; samuel.kounaves@tufts.edu
NR 3
TC 0
Z9 0
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A393
EP A393
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401162
ER
PT J
AU Huberty, JM
Konishi, H
Fournelle, JH
Heck, PR
Valley, JW
Xu, H
AF Huberty, J. M.
Konishi, H.
Fournelle, J. H.
Heck, P. R.
Valley, J. W.
Xu, H.
TI Silician magnetite from the Dales Gorge Banded Iron Formation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Huberty, J. M.; Konishi, H.; Fournelle, J. H.; Heck, P. R.; Valley, J. W.; Xu, H.] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
[Heck, P. R.] Field Museum, Dept Geol, Chicago, IL 60605 USA.
EM jason@geology.wisc.edu
RI Valley, John/B-3466-2011; Heck, Philipp/C-6092-2012
OI Valley, John/0000-0003-3530-2722;
NR 3
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A434
EP A434
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401243
ER
PT J
AU Hurowitz, JA
Fischer, WW
Tosca, NJ
Milliken, RE
AF Hurowitz, J. A.
Fischer, W. W.
Tosca, N. J.
Milliken, R. E.
TI Fe-redox, aridification, and acidic surface waters on early Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Hurowitz, J. A.; Milliken, R. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fischer, W. W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Tosca, N. J.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.
NR 4
TC 0
Z9 0
U1 1
U2 8
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 JUN
PY 2010
VL 74
IS 12
SU 1
BP A439
EP A439
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401254
ER
PT J
AU Johnson, JR
Ashley, J
Bell, JF
Farrand, W
Fleischer, I
Jolliff, B
Herkenhoff, K
Yen, A
AF Johnson, J. R.
Ashley, J.
Bell, J. F., III
Farrand, W.
Fleischer, I.
Jolliff, B.
Herkenhoff, K.
Yen, A.
TI Surface alteration of Fe-Ni meteorites analyzed by the Opportunity Mars
Exploration Rover
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Johnson, J. R.; Herkenhoff, K.] Astrogeol Sci Ctr, USGS, Flagstaff, AZ 86001 USA.
[Ashley, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Bell, J. F., III] Cornell Univ, Dept Astron, Astron, Ithaca, NY 14853 USA.
[Farrand, W.] Space Sci Inst, Boulder, CO 80301 USA.
[Fleischer, I.] Inst Anorgan & Analyt Chem, D-55128 Mainz, Germany.
[Jolliff, B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Yen, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
EM jrjohnson@usgs.gov; James.Ashley@asu.edu; jfb8@cornell.edu;
farrand@SpaceScience.org; irisflei@students.uni-mainz.de;
blj@levee.wustl.edu; kherkenhoff@usgs.gov; albert.s.yen@jpl.nasa.gov
RI Johnson, Jeffrey/F-3972-2015
NR 0
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A473
EP A473
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401515
ER
PT J
AU Jolliff, BL
Shearer, CK
Papanastassiou, DA
AF Jolliff, B. L.
Shearer, C. K.
Papanastassiou, D. A.
TI Analysis of samples from regolith in the Moon's South Pole-Aitken Basin
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Jolliff, B. L.] Washington Univ, St Louis, MO 63130 USA.
[Shearer, C. K.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Papanastassiou, D. A.] Jet Prop Lab, Pasadena, CA 91109 USA.
EM blj@wustl.edu; cshearer@unm.edu; dimitri.a.papanastassiou@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A476
EP A476
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401522
ER
PT J
AU Jones, JH
AF Jones, J. H.
TI Olivine/liquid partitioning, heats of fusion, and the illusion of
linearity
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Jones, J. H.] NASA, Lyndon B Johnson Space Ctr, KR, Houston, TX 77058 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A480
EP A480
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401529
ER
PT J
AU Kuhlman, KR
Garrison, DH
Hiroi, T
Pieters, C
AF Kuhlman, K. R.
Garrison, D. H.
Hiroi, T.
Pieters, C.
TI Lunar space weathering via exposure to ultraviolet radiation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Garrison, D. H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Hiroi, T.; Pieters, C.] Brown Univ, Dept Geo Sci, Providence, RI 02912 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A543
EP A543
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401656
ER
PT J
AU Li, WQ
Beard, BL
Johnson, CM
AF Li, Weiqiang
Beard, Brian L.
Johnson, Clark M.
TI Mg isotope exchange rate and fractionation factor between epsomite and
aqueous solution constrained by three isotope method
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Li, Weiqiang; Beard, Brian L.; Johnson, Clark M.] Univ Wisconsin, Madison, WI 53706 USA.
[Li, Weiqiang; Beard, Brian L.; Johnson, Clark M.] NASA, Astrobiol Inst, Washington, DC USA.
EM wli@geology.wisc.edu
NR 2
TC 0
Z9 0
U1 2
U2 5
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 JUN
PY 2010
VL 74
IS 12
SU 1
BP A594
EP A594
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941401757
ER
PT J
AU Marais, DJD
AF Marais, D. J. Des
CA Athena Sci Team
TI Potentially habitable ancient environments in Gusev crater, Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Marais, D. J. Des; Athena Sci Team] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
EM david.j.desmarais@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A227
EP A227
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400704
ER
PT J
AU McClain, CR
Bontempi, P
Maring, H
AF McClain, Charles R.
Bontempi, Paula
Maring, Hal
TI The NASA decadal survey aerosol, cloud, ecosystems mission
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA.
[Bontempi, Paula; Maring, Hal] NASA Headquarters, Sci Mission Directorate, Washington, DC 20546 USA.
EM charles.r.mcclain@nasa.gov; paula.bontempi@nasa.gov; hal.maring@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A685
EP A685
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402073
ER
PT J
AU McCollom, TM
Bach, W
Hoehler, T
AF McCollom, T. M.
Bach, W.
Hoehler, T.
TI Hydrogen generation for microbial activity in ultramafic-hosted
hydrothermal systems
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [McCollom, T. M.] Univ Colorado, Lab Atmospher & Space Phys, CB392, Boulder, CO 80309 USA.
[Bach, W.] Univ Bremen, Dept Geosci, D-28334 Bremen, Germany.
[Hoehler, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM mccollom@lasp.colorado.edu
NR 10
TC 0
Z9 0
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A686
EP A686
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402076
ER
PT J
AU Mills, B
Boyle, R
Goldblatt, C
Lenton, T
Watson, A
AF Mills, Benjamin
Boyle, Richard
Goldblatt, Colin
Lenton, Timothy
Watson, Andrew
TI What happened in the Neoproterozoic? Investigations using a simplified
Earth system model
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Mills, Benjamin; Boyle, Richard; Lenton, Timothy; Watson, Andrew] Univ E Anglia, Norwich NR4 7TJ, Norfolk, England.
[Goldblatt, Colin] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
EM b.mills@uea.ac.uk
NR 8
TC 0
Z9 0
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A711
EP A711
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402125
ER
PT J
AU Mittlefehldt, DW
AF Mittlefehldt, David W.
TI Asteroidal differentiation - the record in meteorites
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Astromaterials Res Off, Houston, TX 77059 USA.
EM david.w.mittlefehldt@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A715
EP A715
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402133
ER
PT J
AU Nakamura, N
Nyquist, L
Reese, Y
Shih, CY
AF Nakamura, N.
Nyquist, L.
Reese, Y.
Shih, C. -Y.
TI Stable chlorine isotope study of standard rocks and Allende meteorite by
TIMS
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Nakamura, N.; Nyquist, L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Reese, Y.] ESCG Muniz Engn, Houston, TX 77058 USA.
[Shih, C. -Y.] ESCG Jacobs Sverdrup, Houston, TX 77058 USA.
EM noboru.nakamura@nasa.gov
NR 5
TC 0
Z9 0
U1 3
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A745
EP A745
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402194
ER
PT J
AU Oehler, DZ
Robert, F
Walter, MR
Sugitani, K
Meibom, A
Mostefaoui, S
Gibson, E
AF Oehler, D. Z.
Robert, F.
Walter, M. R.
Sugitani, K.
Meibom, A.
Mostefaoui, S.
Gibson, E.
TI Biological diversity in the Archean: New results from NanoSIMS
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Oehler, D. Z.; Gibson, E.] NASA Johnson Space Ctr, Houston, TX USA.
[Robert, F.; Meibom, A.; Mostefaoui, S.] Museum Natl Hist Nat, Lab Mineral & Cosmochim, F-75231 Paris, France.
[Walter, M. R.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Sugitani, K.] Nagoya Univ, Dept Environ Engn & Architecture, Nagoya, Aichi 4648601, Japan.
EM dorothy.z.oehler@nasa.gov; robert@mnhn.fr; malcolm.walter@unsw.edu.au;
sugi@info.human.nagoya-u.ac.jp
NR 3
TC 0
Z9 0
U1 0
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A771
EP A771
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402246
ER
PT J
AU Ohmoto, H
Bevacqua, DC
Johnson, I
Watanabe, Y
AF Ohmoto, Hiroshi
Bevacqua, David C.
Johnson, Ian
Watanabe, Yumiko
TI Geochemical cycles of Fe, Mo, U, Cu, Cr, REEs, and S during the period
3.5-3.2 Ga ago
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16803 USA.
Penn State Univ, Dept Geosci, University Pk, PA 16803 USA.
EM hqo@psu.edu
NR 0
TC 1
Z9 1
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A774
EP A774
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402251
ER
PT J
AU Peslier, AH
Woodland, AB
Lazarov, M
AF Peslier, A. H.
Woodland, A. B.
Lazarov, M.
TI Controls of H incorporation in pyroxenes and garnets from FTIR data on
Kaapvaal craton xenoliths
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Peslier, A. H.] ESCG, Jacobs Technol, Houston, TX 77058 USA.
[Peslier, A. H.] NASA JSC, ARES, Houston, TX 77058 USA.
[Woodland, A. B.; Lazarov, M.] U Frankfurt, D-60438 Frankfurt, Germany.
EM anne.h.peslier@nasa.gov
RI Peslier, Anne/F-3956-2010
NR 8
TC 1
Z9 1
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A808
EP A808
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402320
ER
PT J
AU Quinn, RC
Grunthaner, FJ
Mielke, RE
Chun, WW
White, VE
AF Quinn, R. C.
Grunthaner, F. J.
Mielke, R. E.
Chun, W. W.
White, V. E.
TI In situ fabrication of chemical sensing arrays in extreme environments
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Quinn, R. C.] NASA Ames, SETI Inst, Moffett Field, CA 94035 USA.
[Grunthaner, F. J.; Mielke, R. E.; Chun, W. W.; White, V. E.] NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM Richard.C.Quinn@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A842
EP A842
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402387
ER
PT J
AU Schrader, CM
Cohen, BA
AF Schrader, C. M.
Cohen, B. A.
TI Petrology of the crystalline rocks hosting the Santa Fe impact structure
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Schrader, C. M.] Oak Ridge Associated Univ, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Cohen, B. A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM Christian.M.Schrader@nasa.gov
NR 3
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A927
EP A927
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402557
ER
PT J
AU Singer, SW
Woebken, D
Burow, LC
Prufert-Bebout, L
Bebout, BM
Pett-Ridge, J
Spormann, AM
Weber, PK
AF Singer, Steven W.
Woebken, Dagmar
Burow, Luke C.
Prufert-Bebout, Lee
Bebout, Brad M.
Pett-Ridge, Jennifer
Spormann, Alfred M.
Weber, Peter K.
TI NanoSIP: Combining stable isotope probing and high resolution secondary
ion mass spectrometry to identify diazotrophs in stratified marine
microbial communities
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Singer, Steven W.] Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Woebken, Dagmar; Burow, Luke C.; Spormann, Alfred M.] Stanford Univ, Stanford, CA 94305 USA.
[Prufert-Bebout, Lee; Bebout, Brad M.] NASA, Ames Res Ctr, Washington, DC 20546 USA.
[Pett-Ridge, Jennifer; Spormann, Alfred M.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
EM SWSinger@lbl.gov; dwoebken@stanford.edu; lburow@stanford.edu;
Leslie.E.Bebout@mail.nasa.gov; brad.m.bebout@nasa.gov;
pettridge2@llnl.gov; spormann@stanford.edu; weber21@llnl.gov
RI Abu Laban , Dr. Nidal /E-5809-2011
NR 0
TC 0
Z9 0
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A966
EP A966
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402636
ER
PT J
AU Stern, JC
Mcadam, AC
Franz, HB
Mahaffy, PR
AF Stern, Jennifer C.
Mcadam, Amy C.
Franz, Heather B.
Mahaffy, Paul R.
TI Evolved Gas Analysis coupled with Cavity Ringdown Spectrometry for in
situ delta C-13 measurements of Mars analog materials
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
ID CARBONATE
C1 [Stern, Jennifer C.; Mcadam, Amy C.; Franz, Heather B.; Mahaffy, Paul R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Franz, Heather B.] Univ Maryland, College Pk, MD 20742 USA.
EM Jennifer.C.Stern@nasa.gov
RI McAdam, Amy/E-1556-2012; Stern, Jennifer/E-3135-2012; Franz,
Heather/F-3508-2012
OI Stern, Jennifer/0000-0002-0162-8807;
NR 4
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A993
EP A993
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941402689
ER
PT J
AU Ullman, DJ
Carlson, AE
Legrande, AN
Anslow, FS
Caffee, MW
Licciardi, JM
Syverson, KM
AF Ullman, David J.
Carlson, Anders E.
Legrande, Allegra N.
Anslow, Faron S.
Caffee, Marc W.
Licciardi, Joseph M.
Syverson, Kent M.
TI Testing forcing mechanisms of deglaciation: Cosmogenic dating of
Laurentide Ice Sheet retreat in Wisconsin and surface mass balance
modeling
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Ullman, David J.; Carlson, Anders E.] Univ WI Madison, Dept Geosci, Madison, WI USA.
[Legrande, Allegra N.] Columbia Univ, CCSR, New York, NY USA.
[Legrande, Allegra N.] Columbia Univ, NASA,GISS, New York, NY USA.
[Anslow, Faron S.] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Caffee, Marc W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Licciardi, Joseph M.] Univ NH, Dept Earth Sci, Durham, NH USA.
[Syverson, Kent M.] Univ WI Eau Claire, Dept Geol, Eau Claire, WI USA.
EM ullman@wisc.edu
RI LeGrande, Allegra/D-8920-2012
OI LeGrande, Allegra/0000-0002-5295-0062
NR 5
TC 0
Z9 0
U1 1
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1063
EP A1063
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400167
ER
PT J
AU van Acken, D
Brandon, AD
AF van Acken, D.
Brandon, A. D.
TI Osmium isotopes in aubrites
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [van Acken, D.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[van Acken, D.; Brandon, A. D.] Univ Houston, Houston, TX 77204 USA.
EM dvanacken@uh.edu; abrandon@uh.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1070
EP A1070
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400181
ER
PT J
AU Vance, S
Christensen, LE
Webster, CR
AF Vance, Steve
Christensen, Lance E.
Webster, Christopher R.
TI In situ measurement of CH3SH on Earth and Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Vance, Steve; Christensen, Lance E.; Webster, Christopher R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM svance@jpl.nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1071
EP A1071
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400183
ER
PT J
AU Wang, YF
Xu, HF
Merino, E
AF Wang, Yifeng
Xu, Huifang
Merino, Enrique
TI Nonlinear dynamics of Banded Iron Formation precipitation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Wang, Yifeng] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[Xu, Huifang] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA.
[Xu, Huifang] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
[Merino, Enrique] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1110
EP A1110
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400261
ER
PT J
AU Willis, PA
Fisher, AM
Greer, HF
Mora, MF
Mair, D
Jiao, H
AF Willis, P. A.
Fisher, A. M.
Greer, H. F.
Mora, M. F.
Mair, D.
Jiao, H.
TI Micro total analysis system development for in situ chemical exploration
of Titan and Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Willis, P. A.; Fisher, A. M.; Greer, H. F.; Mora, M. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mair, D.] Fluigence LLC, Santa Clara, CA 95054 USA.
[Jiao, H.] Los Gatos Res Inc, Mountain View, CA 94941 USA.
EM Peter.A.Willis@jpl.nasa.gov
RI Willis, Peter/I-6621-2012
NR 3
TC 0
Z9 0
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1134
EP A1134
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400309
ER
PT J
AU Xu, HF
AF Xu, Huifang
TI Dolomite, dolomitization, and dolomite problem: A new song with old tune
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
NR 0
TC 0
Z9 0
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1160
EP A1160
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400360
ER
PT J
AU Yan, BZ
Han, YM
Peteet, D
AF Yan, Beizhan
Han, Yongming
Peteet, Dorothy
TI Reconstruction of biomass combustion history using black carbon and
polycyclic aromatic hydrocarbons
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Yan, Beizhan] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Han, Yongming] Chinese Acad Sci, Inst Earth Environm, SKLLQG, Xian 710075, Peoples R China.
[Peteet, Dorothy] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RI Han, Yongming/I-8824-2014
NR 0
TC 0
Z9 0
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JUN
PY 2010
VL 74
IS 12
SU 1
BP A1170
EP A1170
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400381
ER
PT J
AU Zahnle, K
Claire, M
Wing, B
AF Zahnle, K.
Claire, M.
Wing, B.
TI Biogenic sulfur gases, MIF-S, and the rise of free oxygen
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Meeting Abstract
CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment
CY JUN 13-18, 2010
CL Knoxville, TN
C1 [Zahnle, K.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Claire, M.] Univ Washington, Dept Astron, Astrobiol Program, Seattle, WA 98195 USA.
[Wing, B.] McGill Univ, Montreal, PQ H3A 2A7, Canada.
EM Kevin.J.Zahnle@NASA.gov; mclaire@astro.washington.edu
NR 0
TC 0
Z9 0
U1 2
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 JUN
PY 2010
VL 74
IS 12
SU 1
BP A1195
EP A1195
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 676TL
UT WOS:000283941400431
ER
PT J
AU Liu, Z
Owen, S
Dong, DA
Lundgren, P
Webb, F
Hetland, E
Simons, M
AF Liu, Zhen
Owen, Susan
Dong, Danan
Lundgren, Paul
Webb, Frank
Hetland, Eric
Simons, Mark
TI Integration of transient strain events with models of plate coupling and
areas of great earthquakes in southwest Japan
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Time-series analysis; Transient deformation; Subduction zone processes
ID SLOW SLIP EVENTS; HIKURANGI SUBDUCTION ZONE; LOW-FREQUENCY EARTHQUAKES;
TIME-DEPENDENT INVERSION; ASEISMIC FAULT SLIP; NANKAI TROUGH; SILENT
SLIP; CRUSTAL DEFORMATION; EPISODIC TREMOR; TOKAI REGION
AB P>We model the crustal deformation caused by two long-term subduction slip transients in southwest Japan, which we refer to as the 2000-2004 Tokai and the 2002-2004 Bungo Channel slow slip events (SSEs). We use re-analysed GEONET position time-series, and a Kalman filter based network inversion method to image the spatiotemporal slip variation of the two events on the plate interface during the period of 1998-2004.67 and 2000-2005. Both events are found to have complex slip histories with multiple subevents. In addition to a newly identified slip subevent in 2002-2003, we find that the major event in the Bungo Channel SSE initiated in early 2003 beneath the northeastern corner of the region and expanded southwestward, in contrast to the slip characteristics suggested by other studies. The re-analysed GPS data in the Tokai region shows a renewed slip activity for the Tokai SSE in early 2003-2004 at a similar location as in the period of 2001-2002. The equivalent M(w) for both the Tokai and Bungo Channel SSEs are about 7.0. Our results show that the Tokai SSE appears to start before the Miyaki-Kozu seismovolcanic event. Integrating plate coupling and SSEs shows that the transient slip zones are located in a region between the locked zones and the epicentres of the low frequency earthquakes (LFEs). At least part of the interseismic slip deficit is released by episodic SSEs beneath the Bungo Channel region. We find excellent temporal correspondence between transient slip and adjacent LFEs for both SSE, suggesting that they are closely related and possibly reflect that long-term slow slip may modulate the occurrence of LFEs.
C1 [Liu, Zhen; Owen, Susan; Dong, Danan; Lundgren, Paul; Webb, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Simons, Mark] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hetland, Eric] Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA.
RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zliu@jpl.nasa.gov
RI Hetland, Eric/D-4297-2012; Simons, Mark/N-4397-2015; Liu,
Zhen/D-8334-2017
OI Simons, Mark/0000-0003-1412-6395;
FU National Aeronautics and Space Administration
FX We thank Kelin Wang for sending us his composite plate geometry model in
his paper. We also thank Akio Katsumata at Meteorological Research
Institute, Japan for sending us LFE catalogue. David Shelly at USGS sent
us his relocated LFE catalogue in western Shikoku. Reviews by Y. Hsu, L.
Wallace, and editor J. Beavan improved this manuscript. The commercial
software Gocad from Paradigm Geophysical (http://www.pdgm.com) was used
in fault surface modelling. 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 and funded through the internal Research and Technology
Development Program.
NR 86
TC 11
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U1 0
U2 6
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0956-540X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD JUN
PY 2010
VL 181
IS 3
BP 1292
EP 1312
DI 10.1111/j.1365-246X.2010.04599.x
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 596WO
UT WOS:000277716400007
ER
PT J
AU Liu, Z
Owen, S
Dong, DA
Lundgren, P
Webb, F
Hetland, E
Simons, M
AF Liu, Zhen
Owen, Susan
Dong, Danan
Lundgren, Paul
Webb, Frank
Hetland, Eric
Simons, Mark
TI Estimation of interplate coupling in the Nankai trough, Japan using GPS
data from 1996 to 2006
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Satellite geodesy; Seismicity and tectonics; Subduction zone processes
ID LOW-FREQUENCY EARTHQUAKES; PHILIPPINE SEA PLATE; ARC-ARC COLLISION;
SOUTHWEST JAPAN; PERMANENT GPS; CRUSTAL DEFORMATION; VELOCITY-FIELD;
SUBDUCTION; SLIP; MODEL
AB P>We used three-component surface velocities in southwest Japan to estimate plate coupling on the subducting plate interface at the Nankai trough. We analyzed continuous GPS data from the Japanese GEONET network from 1996 to 2006 using a consistent analysis strategy that generates bias-fixed solutions for the entire network. We applied systematic time-series analysis methods to estimate common mode error, which improved position solutions for the entire network. To allow for differences in regional deformation sources, we modelled the plate coupling on the plate interface beneath Shikoku island to Kii Peninsula and the Tokai-Suruga trough separately. The results show strong coupling at a depth of similar to 10-30 km off Shikoku and Kii Peninsula. The spatial variation in plate coupling coincides well with the coseismic rupture zones of the past large earthquakes. Maximum slip deficit rates of similar to 2-3 cm yr-1 at the depth of similar to 5-25 km are found beneath the Tokai area, consistent with results from other studies. The downdip limits of the highly coupled areas and transition zones beneath Shikoku and the Kii Peninsula correspond approximately to estimates of the 450 degrees C isotherms. Good correlation is observed between the lateral variations of the slip deficit distribution, low frequency earthquakes, and coseismic slip. This correlation suggests that temperature, and possibly fluid variations, contribute to such correlation in space. The interplate slip deficit derived from the GPS velocities over the 10 yr of observations is generally compatible with the results over shorter time spans, suggesting that plate coupling in SW Japan does not change significantly over the period of these GPS measurements.
C1 [Liu, Zhen; Owen, Susan; Dong, Danan; Lundgren, Paul; Webb, Frank] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Simons, Mark] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hetland, Eric] Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA.
RP Liu, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM zliu@jpl.nasa.gov
RI Hetland, Eric/D-4297-2012; Simons, Mark/N-4397-2015; Liu,
Zhen/D-8334-2017
OI Simons, Mark/0000-0003-1412-6395;
FU National Aeronautics and Space Administration; Gordon and Betty Moore
Foundation
FX We thank K. Wang and Junichi Nakajima for sending us their composite
plate geometry model for the Philippine Sea slab. We thank Akio
Katsumata at Meteorological Research Institute, Japan for providing us
low frequency earthquake catalogue. We also thank GSI for providing us
the raw data of GEONET. Reviews by J. Freymueller, L. Wallace, and
editor J. Beavan improved this manuscript. 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 and funded through the internal Research and
Technology Development Program. This research was supported in part by
the Gordon and Betty Moore Foundation. This is Caltech Tectonic
Observatory Contribution 109.
NR 64
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U1 0
U2 6
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD JUN
PY 2010
VL 181
IS 3
BP 1313
EP 1328
DI 10.1111/j.1365-246X.2010.04600.x
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 596WO
UT WOS:000277716400008
ER
PT J
AU Morishima, R
Stadel, J
Moore, B
AF Morishima, Ryuji
Stadel, Joachim
Moore, Ben
TI From planetesimals to terrestrial planets: N-body simulations including
the effects of nebular gas and giant planets
SO ICARUS
LA English
DT Article
DE Accretion; Origin, Solar System; Planetary formation; Terrestrial
planets
ID TURBULENT PROTOPLANETARY DISKS; ISOTHERMAL GASEOUS DISK; DYNAMICAL
SHAKE-UP; INNER SOLAR-SYSTEM; ORBITAL EVOLUTION; SECULAR RESONANCE; I
MIGRATION; 3-DIMENSIONAL INTERACTION; TIDAL INTERACTION; CLOSE
ENCOUNTERS
AB We present results from a suite of N-body simulations that follow the formation and accretion history of the terrestrial planets using a new parallel treecode that we have developed. We initially place 2000 equal size planetesimals between 0.5 and 4.0 AU and the collisional growth is followed until the completion of planetary accretion (>100 Myr). A total of 64 simulations were carried out to explore sensitivity to the key parameters and initial conditions. All the important effect of gas in laminar disks are taken into account: the aerodynamic gas drag, the disk-planet interaction including Type I migration, and the global disk potential which causes inward migration of secular resonances as the gas dissipates. We vary the initial total mass and spatial distribution of the planetesimals, the time scale of dissipation of nebular gas (which dissipates uniformly in space and exponentially in time), and orbits of Jupiter and Saturn. We end up with 1-5 planets in the terrestrial region. In order to maintain sufficient mass in this region in the presence of Type I migration, the time scale of gas dissipation needs to be 1-2 Myr. The final configurations and collisional histories strongly depend on the orbital eccentricity of Jupiter. If today's eccentricity of Jupiter is used, then most of bodies in the asteroidal region are swept up within the terrestrial region owing to the inward migration of the secular resonance, and giant impacts between protoplanets occur most commonly around 10 Myr. If the orbital eccentricity of Jupiter is close to zero, as suggested in the Nice model, the effect of the secular resonance is negligible and a large amount of mass stays for a long period of time in the asteroidal region. With a circular orbit for Jupiter, giant impacts usually occur around 100 Myr, consistent with the accretion time scale indicated from isotope records. However, we inevitably have an Earth size planet at around 2 AU in this case. It is very difficult to obtain spatially concentrated terrestrial planets together with very late giant impacts, as long as we include all the above effects of gas and assume initial disks similar to the minimum mass solar nebular. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Morishima, Ryuji] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90065 USA.
[Stadel, Joachim; Moore, Ben] Univ Zurich, Inst Theoret Phys, CH-8006 Zurich, Switzerland.
RP Morishima, R (reprint author), CALTECH, Jet Prop Lab, M-S 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ryuji.morishima@jpl.nasa.gov
NR 82
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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 JUN
PY 2010
VL 207
IS 2
BP 517
EP 535
DI 10.1016/j.icarus.2009.11.038
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900003
ER
PT J
AU Kahre, MA
Haberle, RM
AF Kahre, Melinda A.
Haberle, Robert M.
TI Mars CO2 cycle: Effects of airborne dust and polar cap ice emissivity
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Mars, Surface; Mars, Polar caps
ID SEASONAL CO-2 CYCLE; MARTIAN ATMOSPHERE; GENERAL-CIRCULATION;
INTERANNUAL VARIABILITY; PHYSICAL-PROPERTIES; VIKING OBSERVATIONS;
SURFACE PRESSURE; SIMULATIONS; STORMS; HYDROGEN
AB Mars General Circulation Model (GCM) simulations are presented to illustrate the importance of the ice emissivity of the seasonal CO2 polar caps in regulating the effects of airborne dust on the martian CO2 cycle. Simulated results show that atmospheric dust suppresses CO2 condensation when the CO2 ice emissivity is high but enhances it when the CO2 ice emissivity is low. This raises the possibility that the reason for the repeatable nature of the CO2 cycle in the presence of a highly variable dust cycle is that the CO2 ice emissivity is "neutral" - the value that leads to no change in CO2 condensation with changing atmospheric dust. For this GCM, the "neutral" emissivity is approximately 0.55, which is low compared to observed cap emissivities. This inconsistency poses a problem for this hypothesis. However, it is clear that the CO2 ice emissivity is a critical physical parameter in determining how atmospheric dust affects the CO2 cycle on Mars. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Kahre, Melinda A.; Haberle, Robert M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kahre, Melinda A.] Bay Area Environm Res Ctr, Moffett Field, CA 94035 USA.
RP Kahre, MA (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM melinda.a.kahre@nasa.gov
FU NASA
FX This project was supported by NASA's Postdoctoral Program (NPP) and
NASA's Planetary Atmospheres Program.
NR 36
TC 12
Z9 12
U1 0
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2010
VL 207
IS 2
BP 648
EP 653
DI 10.1016/j.icarus.2009.12.016
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900016
ER
PT J
AU Roach, LH
Mustard, JF
Lane, MD
Bishop, JL
Murchie, SL
AF Roach, Leah H.
Mustard, John F.
Lane, Melissa D.
Bishop, Janice L.
Murchie, Scott L.
TI Diagenetic haematite and sulfate assemblages in Valles Marineris
SO ICARUS
LA English
DT Article
DE Mars, Surface; Spectroscopy; Mineralogy
ID THERMAL EMISSION SPECTROMETER; MERIDIANI-PLANUM; LAYERED DEPOSITS;
CRYSTALLINE HEMATITE; WEATHERING PRODUCTS; MARS PATHFINDER; BURNS
FORMATION; SURFACE; MINERALOGY; STRATIGRAPHY
AB Previous orbital mapping of crystalline gray haematite, ferric oxides, and sulfates has shown an association of this mineralogy with light-toned, layered deposits on the floor of Valles Marineris, in chaos terrains in the canyon's outflow channels, and in Meridiani Planum. The exact nature of the relationship between ferric oxides and sulfates within Valles Marineris is uncertain. The Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) spectrometer initially identified sulfate and ferric oxides in the layered deposits of Valles Marineris. The Thermal Emission Spectrometer (TES) has also mapped coarse (gray) haematite in or at the base of these deposits. We use Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) spectra and Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) imagery from the Mars Reconnaissance Orbiter (MRO) to explore the mineralogy and morphology of the large layered deposit in central Capri Chasma, part of the Valles Marineris canyon system that has large, clear exposures of sulfate and haematite. We find kieserite (MgSO4 center dot H2O) and ferric oxide (often crystalline red haematite) in the lower bedrock exposures and a polyhydrated sulfate without ferric oxides in the upper bedrock. This stratigraphy is duplicated in many other basinal chasmata, suggesting a common genesis. We propose the haematite and monohydrated sulfate formed by diagenetic alteration of a sulfate-rich sedimentary deposit, where the upper polyhydrated sulfate-rich, haematite-poor layers either were not buried sufficiently to convert to a monohydrated sulfate or were part of a later depositional phase. Based on the similarities between the Valles Marineris assemblages and the sulfate and haematite-rich deposits of Meridiani Planum, we hypothesize a common evaporite and diagenetic formation process for the Meridiani Planum sediments and the sulfate-bearing basinal Interior Layered Deposits. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Roach, Leah H.; Mustard, John F.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Lane, Melissa D.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA.
[Bishop, Janice L.] NASA, Ames Res Ctr, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Roach, LH (reprint author), Brown Univ, Dept Geol Sci, 324 Brook St, Providence, RI 02912 USA.
EM leah_roach@brown.edu
RI Murchie, Scott/E-8030-2015
OI Murchie, Scott/0000-0002-1616-8751
NR 93
TC 34
Z9 34
U1 1
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2010
VL 207
IS 2
BP 659
EP 674
DI 10.1016/j.icarus.2009.11.029
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900018
ER
PT J
AU Marion, GM
Catling, DC
Zahnle, KJ
Claire, MW
AF Marion, G. M.
Catling, D. C.
Zahnle, K. J.
Claire, M. W.
TI Modeling aqueous perchlorate chemistries with applications to Mars
SO ICARUS
LA English
DT Article
DE Cosmochemistry; Geological processes; Mars, Surface; Mineralogy
ID PHOENIX LANDING SITE; MERIDIANI-PLANUM; LOW-TEMPERATURES; MINERAL
SOLUBILITIES; IRON CHEMISTRY; SYSTEM; EQUILIBRIA; 25-DEGREES-C;
CARBONATE; JAROSITE
AB NASA's Phoenix lander identified perchlorate and carbonate salts on Mars. Perchlorates are rare on Earth, and carbonates have largely been ignored on Mars following the discovery by NASA's Mars Exploration Rovers of acidic precipitated minerals such as jarosite. In light of the Phoenix results, we updated the aqueous thermodynamic model FREZCHEM to include perchlorate chemistry. FREZCHEM models the Na-K-Mg-Ca-Fe(II)-Fe(III)-Al-H-Cl-Br-SO4-NO3-OH-HCO3-CO3-CO2-O-2-CH4-Si-H2O system, with 95 solid phases. We added six perchlorate salts: NaClO4 center dot H2O, NaClO4 center dot 2H(2)O, KClO4, Mg(ClO4)(2)center dot 6H(2)O, Mg(ClO4)(2)center dot 8H(2)O, and Ca(ClO4)(2)center dot 6H(2)O. Modeled eutectic temperatures for Na, Mg, and Ca perchlorates ranged from 199 K (-74 degrees C) to 239 K (-34 degrees C) in agreement with experimental data.
We applied FREZCHEM to the average solution chemistry measured by the Wet Chemistry Laboratory (WCL) experiment at the Phoenix site when soil was added to water. FREZCHEM was used to estimate SO42- and alkalinity concentrations that were missing from the WCL data. The amount of SO42- is low compared to estimates from elemental abundance made by other studies on Mars. In the charge-balanced solution, the dominant cations were Mg2+ and Na+ and the dominant anions were ClO4-, SO42-, and alkalinity. The abundance of calcite measured at the Phoenix site has been used to infer that the soil may have been subject to liquid water in the past, albeit not necessarily locally; so we used FREZCHEM to evaporate (at 280.65 K) and freeze (from 280.65 to 213.15 K) the WCL-measured solution to provide insight into salts that may have been in the soil. Salts that precipitated under both evaporation and freezing were calcite, hydromagnesite, gypsum, KClO4, and Mg(ClO4)(2)center dot 8H(2)O. Epsomite (MgSO4 center dot 7H(2)O) and NaClO4 center dot H2O were favored by evaporation at temperatures >0 degrees C, while meridianite (MgSO4 center dot 11H(2)O), MgCl2 center dot 12H(2)O, and NaClO4 center dot 2H(2)O were favored at subzero temperatures. Incongruent melting of such highly hydrated salts could be responsible for vug formation elsewhere on Mars.
All K+ precipitated as insoluble KClO4 during both evaporation and freezing simulations, accounting for 15.8% of the total perchlorates. During evaporation, 35.8% of perchlorates precipitated with Na+ and 48.4% with Mg2+. During freezing, 58.4% precipitated with Na+ and 24.8% with Mg2+. Given its low eutectic temperature, the existence of Mg(ClO4)(2) in either case allows for the possibility of liquid brines on Mars today. FREZCHEM also showed that Ca(ClO4)(2) would likely not have precipitated at the Phoenix landing site due to the strong competing sinks for Ca as calcite and gypsum. Overall, these results help constrain the salt mineralogy of the soil. Differences between evaporites and cryogenites suggest ways to discriminate between evaporation and freezing during salt formation. Future efforts, such as sample return or in situ X-ray diffraction, may make such a determination possible. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Marion, G. M.] Desert Res Inst, Reno, NV 89512 USA.
[Catling, D. C.; Claire, M. W.] Univ Washington, Seattle, WA 98195 USA.
[Zahnle, K. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Marion, GM (reprint author), Desert Res Inst, 2215 Raggio Pkwy, Reno, NV 89512 USA.
EM giles.marion@dri.edu
RI Catling, David/D-2082-2009;
OI Catling, David/0000-0001-5646-120X
FU NASA
FX Funding was provided by a NASA DDF project, "Volcanic SO2,
Atmospheric Photochemistry, and Climate on Early Mars." We thank Vincent
Chevrier for assistance in tracking down perchlorate data sources. We
thank Lisa Wable for assistance in preparing the manuscript.
NR 57
TC 43
Z9 43
U1 1
U2 21
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 JUN
PY 2010
VL 207
IS 2
BP 675
EP 685
DI 10.1016/j.icarus.2009.12.003
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900019
ER
PT J
AU Masiero, J
AF Masiero, Joseph
TI Albedo heterogeneity on the surface of (1943) Anteros
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Polarimetry
ID POLARIMETRIC OBSERVATIONS; 4 VESTA; POLARIZATION; TELESCOPE; ASTEROIDS;
LIGHTCURVE
AB We have investigated the effect of rotation on the polarization of scattered light for the near-Earth asteroid (1943) Anteros using the Dual Beam Imaging Polarimeter on the University of Hawaii's 2.2 m telescope. Anteros is an L-type asteroid that has not been previously observed polarimetrically. We find weak but significant variations in the polarization of Anteros as a function of rotation, indicating albedo changes across the surface. Specifically, we find that Anteros has a background albedo of p(v) = 0.18 +/- 0.02 with a dark spot of p(v) < 0.09 covering <2% of the surface. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Masiero, Joseph] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Masiero, Joseph] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Masiero, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 264-767, Pasadena, CA 91106 USA.
EM Joseph.Masiero@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA PAST [NNG06G146G]
FX J.M. was supported under NASA PAST Grant NNG06G146G. The author would
like to thank Rob Jedicke and Alan Tokunaga for providing comments on
the manuscript, as well as V. Rosenbush and an anonymous referee for
helpful reviews that improved the paper. The author wishes to recognize
and acknowledge the very significant cultural role and reverence that
the summit on Mauna Kea has always had within the indigenous Hawaiian
community. I am most fortunate to have the opportunity to conduct
observations from this sacred mountain.
NR 28
TC 4
Z9 4
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 JUN
PY 2010
VL 207
IS 2
BP 795
EP 799
DI 10.1016/j.icarus.2009.12.033
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900027
ER
PT J
AU Vernazza, P
Carry, B
Emery, J
Hora, JL
Cruikshank, D
Binzel, RP
Jackson, J
Helbert, J
Maturilli, A
AF Vernazza, P.
Carry, B.
Emery, J.
Hora, J. L.
Cruikshank, D.
Binzel, R. P.
Jackson, J.
Helbert, J.
Maturilli, A.
TI Mid-infrared spectral variability for compositionally similar asteroids:
Implications for asteroid particle size distributions
SO ICARUS
LA English
DT Article
DE Asteroids, Surfaces; Spectroscopy; Mineralogy; Meteorites
ID THERMAL EMISSION-SPECTROSCOPY; SPITZER-SPACE-TELESCOPE; MAIN BELT
ASTEROIDS; IRRADIANCE CALIBRATION; PARTICULATE SURFACES; MU-M; INFRARED
OBSERVATIONS; REFLECTANCE SPECTRA; ANALOG MATERIALS; 13-MU-M SPECTRA
AB We report an unexpected variability among mid-infrared spectra (IRTF and Spitzer data) of eight S-type asteroids for which all other remote sensing interpretations (e.g. VNIR spectroscopy, albedo) yield similar compositions. Compositional fitting making use of their mid-IR spectra only yields surprising alternative conclusions: (1) these objects are not "compositionally similar" as the inferred abundances of their main surface minerals (olivine and pyroxene) differ from one another by 35% and (2) carbonaceous chondrite and ordinary chondrite meteorites provide an equally good match to each asteroid spectrum.
Following the laboratory work of Ramsey and Christensen (Ramsey, M.S., Christensen, P.R. [1998]. J. Geophys. Res, 103, 577-596), we interpret this variability to be physically caused by differences in surface particle size and/or the effect of space weathering processes. Our results suggest that the observed asteroids must be covered with very fine (<5 mu m) dust that masks some major and most minor spectral features. We speculate that the compositional analysis may be improved with a spectral library containing a wide variety of well characterized spectra (e.g., olivine, orthopyroxene, feldspar, iron, etc.) obtained from very fine powders. In addition to the grain size effect, space weathering processes may contribute as well to the reduction of the spectral contrast. This can be directly tested via new laboratory irradiation experiments. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Vernazza, P.] European Space Agcy, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands.
[Carry, B.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France.
[Carry, B.] European So Observ, Santiago 19, Chile.
[Emery, J.] Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cruikshank, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Binzel, R. P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Jackson, J.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Helbert, J.; Maturilli, A.] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
RP Vernazza, P (reprint author), ESA ESTEC RSSD SCI, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
EM pierre.vernazza@esa.int
OI Helbert, Jorn/0000-0001-5346-9505; Hora, Joseph/0000-0002-5599-4650
NR 84
TC 22
Z9 22
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
EI 1090-2643
J9 ICARUS
JI Icarus
PD JUN
PY 2010
VL 207
IS 2
BP 800
EP 809
DI 10.1016/j.icarus.2010.01.011
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900028
ER
PT J
AU Moore, C
Miki, K
Goldstein, DB
Stapelfeldt, K
Varghese, PL
Trafton, LM
Evans, RW
AF Moore, C.
Miki, K.
Goldstein, D. B.
Stapelfeldt, K.
Varghese, P. L.
Trafton, L. M.
Evans, R. W.
TI Monte Carlo modeling of Io's [OI] 6300 angstrom and [SII] 6716 angstrom
auroral emission in eclipse
SO ICARUS
LA English
DT Article
DE Io; Aurorae; Jupiter, Satellites; Satellites, Atmospheres; Collisional
physics
ID SULFUR-DIOXIDE; PLASMA TORUS; SO2 ATMOSPHERE; ENERGETIC ELECTRONS;
DRIVEN ATMOSPHERE; VOLCANIC PLUMES; CROSS-SECTIONS; UV EMISSIONS; PELE
PLUME; SUBLIMATION
AB We present a Monte Carlo (MC) model of [OI] 6300 angstrom and [SII] 6716 angstrom emission from Io entering eclipse. The simulation accounts for the 3-D distribution of SO(2), O, SO, S, and O(2) in to's atmosphere, several volcanic plumes, and the magnetic field around Io. Thermal electrons from the jovian plasma torus are input along the simulation domain boundaries and move along the magnetic field lines distorted by Io, occasionally participating in collisions with neutrals. We find that the atmospheric asymmetry resulting from varying degrees of atmospheric collapse across Io (due to eclipse ingress) and the presence of volcanoes contributes significantly to the unique morphology of the [OI] 6300 angstrom emission. The [OI] radiation lifetime of similar to 134 s limits the emission to regions that have a sufficiently low neutral density so that intermolecular collisions are rare. We find that at low altitudes (typically <40 km) and in volcanic plumes (Pele, Prometheus, etc.) the number density is large enough (>4 x 10(9) cm(-3)) to collisionally quench nearly all (>95%) of the excited oxygen for reasonable quenching efficiencies. Upstream (relative to the plasma flow), Io's perturbation of the jovian magnetic field mirrors electrons with high pitch angles, while downstream collisions can trap the electrons. This magnetic field perturbation is one of the main physical mechanisms that results in the upstream/downstream brightness asymmetry in [OI] emission seen in the observation by Trauger et al. (Trauger, J.T., Stapelfeldt, K.R., Ballester, G.E., Clarke, J.I., 1997. HST observations of [OI] emissions from Io in eclipse. AAS-DPS Abstract (1997DPS29.1802T)). There are two other main causes for the observed brightness asymmetry. First, the observation's viewing geometry of the wake spot crosses the dayside atmosphere and therefore the wake's observational field of view includes higher oxygen column density than the upstream side. Second, the phased entry into eclipse results in less atmospheric collapse and thus higher collisional quenching on the upstream side relative to the wake. We compute a location (both in altitude and latitude) for the intense wake emission feature that agrees reasonably well with this observation. Furthermore, the peak intensity of the simulated wake feature is less than that observed by a factor of similar to 3, most likely because our model does not include direct dissociation-excitation of SO(2) and SO. We find that the latitudinal location of the emission feature depends not so much on the tilt of the magnetic field as on the relative north/south flux tube depletion that occurs due to Io's changing magnetic latitude in the plasma torus. From 1-D simulations, we also find that the intensity of [SII] 6716 and 6731 angstrom emission is much weaker than that of [OI] even if the [SII] excitation cross section is 10(3) times larger than excitation to [OI]. This is because the density of S(+) is much less than that of O and because the Einstein-A coefficient of the [SII] emission is a factor of similar to 10 smaller than that of [OI]. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Moore, C.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Stapelfeldt, K.; Evans, R. W.] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Moore, C (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, 1 Univ Stn,C0600, Austin, TX 78712 USA.
EM moorech@ices.utexas.edu
RI Stapelfeldt, Karl/D-2721-2012
FU NASA [NAS5-26555, NAG5-11991, NNX08AQ49G]; STScl [HST-AR-10322.01-A]
FX Based on observations with the NASA/ESA Hubble Space Telescope. Archival
research support for Program 9535 was provided by NASA through a grant
from the Space Telescope Science Institute, which is operated by the
Associated Universities for Research in Astronomy, Incorporated, under
NASA Contract NAS5-26555. This work was supported by STScl Grant
HST-AR-10322.01-A and NASA Grants NAG5-11991 and NNX08AQ49G. The authors
acknowledge the Texas Advanced Computing Center (TACC) at The University
of Texas at Austin for providing HPC resources that have contributed to
the research results reported within this paper.
NR 77
TC 7
Z9 7
U1 0
U2 1
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUN
PY 2010
VL 207
IS 2
BP 810
EP 833
DI 10.1016/j.icarus.2010.01.004
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900029
ER
PT J
AU Patterson, GW
Collins, GC
Head, JW
Pappalardo, RT
Prockter, LM
Lucchitta, BK
Kay, JP
AF Patterson, G. Wesley
Collins, Geoffrey C.
Head, James W.
Pappalardo, Robert T.
Prockter, Louise M.
Lucchitta, Baerbel K.
Kay, Jonathan P.
TI Global geological mapping of Ganymede
SO ICARUS
LA English
DT Article
DE Ganymede; Satellites, Surfaces; Jupiter, Satellites
ID GALILEO NOMINAL MISSION; GROOVED TERRAIN; DARK TERRAIN; HIGH-RESOLUTION;
EXTENSIONAL INSTABILITY; CRATERING RATES; IMPACT FEATURES; WATER-ICE;
SATELLITES; JUPITER
AB We have compiled a global geological map of Ganymede that represents the most recent understanding of the satellite based on Galileo mission results. This contribution builds on important previous accomplishments in the study of Ganymede utilizing Voyager data and incorporates the many new discoveries that were brought about by examination of Galileo data. We discuss the material properties of geological units defined utilizing a global mosaic of the surface with a nominal resolution of 1 km/pixel assembled by the USGS with the best available Voyager and Galileo regional coverage and high resolution imagery (100-200 m/pixel) of characteristic features and terrain types obtained by the Galileo spacecraft. We also use crater density measurements obtained from our mapping efforts to examine age relationships amongst the various defined units. These efforts have resulted in a more complete understanding of the major geological processes operating on Ganymede, especially the roles of cryovolcanic and tectonic processes in the formation of might materials. They have also clarified the characteristics of the geological units that comprise the satellite's surface, the stratigraphic relationships of those geological units and structures, and the geological history inferred from those relationships. For instance, the characteristics and stratigraphic relationships of dark lineated material and reticulate material suggest they represent an intermediate stage between dark cratered material and light material units. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Patterson, G. Wesley] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
[Collins, Geoffrey C.; Kay, Jonathan P.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA.
[Patterson, G. Wesley; Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lucchitta, Baerbel K.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Kay, Jonathan P.] Univ Idaho, Dept Geol Sci, Moscow, ID 83844 USA.
RP Patterson, GW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, MP3-E106,11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM wes.patterson@jhuapl.edu
FU NASA [NNG05GJ787G]
FX We thank Ken Tanaka and Jeff Moore for their careful review of this
manuscript and the useful comments they provided. This work was
supported under a grant awarded through NASA's Planetary Geology and
Geophysics program (NNG05GJ787G).
NR 71
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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 JUN
PY 2010
VL 207
IS 2
BP 845
EP 867
DI 10.1016/j.icarus.2009.11.035
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900031
ER
PT J
AU Hasenkopf, CA
Beaver, MR
Trainer, MG
Dewitt, HL
Freedman, MA
Toon, OB
McKay, CP
Tolbert, MA
AF Hasenkopf, Christa A.
Beaver, Melinda R.
Trainer, Melissa G.
Dewitt, H. Langley
Freedman, Miriam A.
Toon, Owen B.
McKay, Christopher P.
Tolbert, Margaret A.
TI Optical properties of Titan and early Earth haze laboratory analogs in
the mid-visible
SO ICARUS
LA English
DT Article
DE Titan; Spectroscopy; Experimental techniques; Photochemistry
ID COMPLEX REFRACTIVE-INDEX; CAVITY RING; EARLY ATMOSPHERE; ORGANIC HAZE;
AEROSOL SPECTROMETER; MODEL; SPECTROSCOPY; GREENHOUSE; PHOTOCHEMISTRY;
METHANE
AB Scattering and absorption of sunlight by aerosols are integral to understanding the radiative balance of any planetary atmosphere covered in a haze, such as Titan and possibly the early Earth. One key optical parameter of an aerosol is its refractive index. We have simulated both Titan and early Earth organic haze aerosols in the laboratory and measured the real and imaginary portion of their refractive index at lambda = 532 nm using cavity ringdown aerosol extinction spectroscopy. This novel technique allows analysis on freely-floating particles minutes after formation. For our Titan analog particles, we find a real refractive index of n = 1.35 +/- 0.01 and an imaginary refractive index k = 0.023 +/- 0.007, and for the early Earth analog particles we find n = 1.81 +/- 0.02 and k = 0.055 +/- 0.020. The Titan analog refractive index has a smaller real and similar imaginary refractive index compared to most previous laboratory measurements of Titan analog films, including values from Khare et al. (Khare, B.N., Sagan, C., Arakawa, E.T., Suits, F., Callcott, TA., Williams, M.W. [1984]. Icarus 60, 127-137). These newly measured Titan analog values have implications for spacecraft retrievals of aerosol properties on Titan. The early Earth analog has a significantly higher real and imaginary refractive index than Titan analogs reported in the literature. These differences suggest that, for a given amount of aerosol, the early Earth analog would act as a stronger anti-greenhouse agent than the Titan analog. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Hasenkopf, Christa A.; Beaver, Melinda R.; Dewitt, H. Langley; Freedman, Miriam A.; Tolbert, Margaret A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Hasenkopf, Christa A.; Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Beaver, Melinda R.; Dewitt, H. Langley; Tolbert, Margaret A.] Univ Colorado, Dept Chem, Boulder, CO 80309 USA.
[Trainer, Melissa G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Toon, Owen B.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[McKay, Christopher P.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94503 USA.
RP Hasenkopf, CA (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM Christa.Hasenkopf@colorado.edu
RI Trainer, Melissa/E-1477-2012; Freedman, Miriam/A-4571-2013
OI Freedman, Miriam/0000-0003-4374-6518
FU NASA [NNX07AV55G, NNX07AF190, NNX08AG93G, NNX09AE12G]; National Science
Foundation; EPA; NOAA
FX This material is based on work supported by NASA Grants NNX07AV55G,
NNX07AF190, NNX08AG93G, and NNX09AE12G. CAH was supported with a
National Science Foundation Graduate Research Fellowship. MRB was
supported by an EPA-STAR fellowship. MGT was supported by an appointment
to the NASA Postdoctoral Program at the University of Colorado Center
for Astrobiology administered by Oak Ridge Associated Universities. HLD
is supported through a NASA-GSRP fellowship. MAF acknowledges support
from the NOAA Climate and Global Change Postdoctoral Fellowship Program
administered by the University of Corporation for Atmospheric Research.
NR 47
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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 JUN
PY 2010
VL 207
IS 2
BP 903
EP 913
DI 10.1016/j.icarus.2009.12.015
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900034
ER
PT J
AU Anderson, CM
Samuelson, RE
Bjoraker, GL
Achterberg, RK
AF Anderson, C. M.
Samuelson, R. E.
Bjoraker, G. L.
Achterberg, R. K.
TI Particle size and abundance of HC3N ice in Titan's lower stratosphere at
high northern latitudes
SO ICARUS
LA English
DT Article
DE Titan; Radiative transfer
ID COMPOSITE INFRARED SPECTROMETER; SPECTROSCOPIC DATABASE; POLAR
STRATOSPHERE; ABSORPTION-SPECTRA; CLOUDS; TEMPERATURES; ATMOSPHERE;
PAIRS; TROPOSPHERE; SURFACE
AB Up to now, there has been no corroboration from Cassini CIRS of the Voyager IRIS-discovery of cyanoacetylene (HC3N) ice in Titan's thermal infrared spectrum. We report the first compelling spectral evidence from CIRS for the v(6) HC3N ice feature at 506 cm(-1) at latitudes 62 degrees N and 70 degrees N, from which we derive particle sizes and column abundances in Titan's lower stratosphere. We find mean particle radii of 3.0 mu m and 2.3 mu m for condensed HC3N at 62 degrees N and 70 degrees N, respectively, and corresponding ice phase molecular column abundances in the range 1-10 x 10(16) mol cm(-2). Only upper limits for cloud abundances can be established at latitudes of 85 degrees N, 55 degrees N, 30 degrees N, 10 degrees N, and 15 degrees S. Under the assumption that cloud tops coincide with the uppermost levels at which HC3N vapor saturates, we infer geometric thicknesses for the clouds equivalent to 10-20 km or so, with tops at 165 km and 150 km at 70 degrees N and 62 degrees N, respectively. Published by Elsevier Inc.
C1 [Anderson, C. M.; Bjoraker, G. L.] NASA, GSFC, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Samuelson, R. E.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Anderson, CM (reprint author), NASA, GSFC, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM carrie.m.anderson@nasa.gov
RI Anderson, Carrie/C-8097-2012; Bjoraker, Gordon/D-5032-2012
FU Cassini project; Goddard Space Flight Center
FX We would like to extend our thanks to F.M. Flasar for his useful
comments concerning an initial draft of this paper. This research was
supported in part by the Cassini project and 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. Perceptive remarks by two anonymous referres led to
considerable improvement in the analysis.
NR 30
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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 JUN
PY 2010
VL 207
IS 2
BP 914
EP 922
DI 10.1016/j.icarus.2009.12.024
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900035
ER
PT J
AU Le Gall, A
Janssen, MA
Paillou, P
Lorenz, RD
Wall, SD
AF Le Gall, A.
Janssen, M. A.
Paillou, P.
Lorenz, R. D.
Wall, S. D.
CA Cassini Radar Team
TI Radar-bright channels on Titan
SO ICARUS
LA English
DT Article
DE Titan; Radar observations; Radio observations; Satellites, Surfaces;
Geological processes
ID HUYGENS LANDING SITE; CASSINI RADAR; LIGHT-SCATTERING; REFRACTION
SCATTERING; SPHEROIDAL PARTICLES; COHERENT BACKSCATTER; BACK-SCATTERING;
SATURNS RINGS; SURFACE; SATELLITES
AB During Cassini's T44 flyby of Titan (May 28, 2008), the Cassini SAR (synthetic aperture radar) revealed sinuous channels in the Southwest of Xanadu. These channels feature very large radar cross-sections, up to 5 dB, whereas the angle of incidence was relatively high, similar to 20 degrees. This backscatter is larger than allowed by the coherent backscatter model considered to explain the unusual reflective and polarization properties of the icy satellites and only a few radar scattering mechanisms can be responsible for such high radar returns. The presence of rounded (icy) pebbles with size larger than the radar wavelength (2.18 cm) is proposed to explain the large radar cross-sections measured in these units. The radar-bright channels are thus interpreted as riverbeds, where debris, likely shaped and transported by fluvial activity, have been deposited. Similar debris were observed in the landing site of the Huygens probe. This work may point the way to an explanation for the enhanced brightness of other fluvial regions of Titan. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Le Gall, A.; Janssen, M. A.; Wall, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Paillou, P.] Univ Bordeaux 1, Observ Aquitain Sci Univers, F-33271 Floirac, France.
[Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Dept Space, Laurel, MD 20723 USA.
RP Le Gall, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alice.Le.Gall@jpl.nasa.gov
RI Lorenz, Ralph/B-8759-2016
OI Lorenz, Ralph/0000-0001-8528-4644
FU NASA
FX We gratefully acknowledge those who designed, developed and operate the
Cassini/Huygens mission, which is a joint endeavor of NASA, the European
Space Agency (ESA), and the Italian Space Agency (ASI) and is managed by
JPL/Caltech under a contract with NASA. 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. The authors wish to thank H.U. Keller and M.
Kuppers for sharing their size statistic analysis of the pebbles of the
Huygens landing site. Fig. 7 is extracted from Keller et al. (2008).
They are also grateful to Alain Reineix and Christophe Guiffaut from
XLIM, Limoges, France who designed the TEMSI-FD code and whish to thank
two anonymous reviewers for their insightful and thorough reviews. A. Le
Gall is supported by the NASA Postdoctoral Program, administrated by Oak
Ridge Associated Universities.
NR 77
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD JUN
PY 2010
VL 207
IS 2
BP 948
EP 958
DI 10.1016/j.icarus.2009.12.027
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900039
ER
PT J
AU Robuchon, G
Choblet, G
Tobie, G
Cadek, O
Sotin, C
Grasset, O
AF Robuchon, G.
Choblet, G.
Tobie, G.
Cadek, O.
Sotin, C.
Grasset, O.
TI Coupling of thermal evolution and despinning of early Iapetus
SO ICARUS
LA English
DT Article
DE Ices; Iapetus; Interiors; Thermal histories; Rotational dynamics
ID TEMPERATURE-DEPENDENT VISCOSITY; EARLY SOLAR-SYSTEM; ICY SATELLITES;
GALILEAN SATELLITES; POLYCRYSTALLINE ICE; INTERNAL STRUCTURE; EQUATORIAL
RIDGE; CONVECTION; ORIGIN; MANTLE
AB The Cassini mission revealed two spectacular characteristics of Iapetus: (1) a geologically old and high equatorial ridge, which is unique in the Solar System and (2) a large flattening of 35 km consistent with the equilibrium figure for a hydrostatic body rotating with a period of 1611, whereas the current spin period is 79.33 days. This study describes three-dimensional simulations of solid-state convection within an undifferentiated Iapetus. It investigates the implications for the evolution of the interior thermal structure and its spin rate and global shape using radially layered viscoelastic models. The role of the concentration in the short-lived radiogenic element [(26)Al], just after accretion is completed, is specifically addressed. The first result is to show that whatever the [(26)Al] value, convection occurs. As suggested by Castillo-Rogez et al. [Castillo-Rogez, J., Matson, D., Sotin, C., Johnson, T., Lunine, J., Thomas, P. [2007] Icarus, 190, 179-202], convection reduces the warming of the interior compared to the conductive evolution and therefore limits the conditions for despinning. In our calculations, two conceptual linear viscoelastic models are used. When considering a Maxwell rheology, the interior temperature (viscosity) never reaches a value high (low) enough to induce despinning. In order to promote dissipation at low temperature, a Burgers rheology, which includes an additional dissipation peak, is introduced. For favorable parameter values, this latter rheology leads to despinning. However, only models associated with large amounts of short-lived radiogenic elements ([(26)Al] >= 25 ppb) lead to the observed flattening. This suggests that the accretion process needs to be completed shortly after the formation of CAIs (Calcium-Aluminum-rich Inclusions) (<= 4 Myr). For[(26)Al] varying between 72 and 46 ppb, the observed flattening is obtained only for a limited range of initial spin period, between 9.5 and 10.2 h. For [(26)Al] ranging between 30 and 15 ppb, initial spin rates smaller than 8.5 h are required. For smaller values of [(26)Al], the body is too cold and viscous to acquire a significant flattening even if a rotation period close to the body disruption limit is considered. Even with a thin lithosphere during the early stage, our simulations show that Iapetus never reaches the equilibrium figure for a hydrostatic body due to the non-zero rigidity of the lithosphere. The 35 km value of the flattening is the result of the partial relaxation of an ancient larger flattening ranging between 45 and 80 km, depending on the evolution of the lithosphere thickness mainly controlled by the radiogenic content. A thin lithosphere is consistent with an early building of the equatorial ridge. The lithosphere thickening due to interior cooling can explain the preservation of the ridge throughout the remaining evolution of Iapetus. (C) 2009 Elsevier Inc. All rights reserved.
C1 [Robuchon, G.; Choblet, G.; Tobie, G.; Grasset, O.] Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France.
[Choblet, G.; Tobie, G.; Grasset, O.] Univ Nantes, CNRS, UMR 6112, F-44322 Nantes, France.
[Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cadek, O.] Charles Univ Prague, Fac Math & Phys, Dept Geophys, Prague, Czech Republic.
RP Robuchon, G (reprint author), Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France.
EM guillaume.robuchon@univ-nantes.fr
RI Cadek, Ondrej/P-6527-2016
OI Cadek, Ondrej/0000-0001-8331-3093
FU Ministry of Education in the Czech Republic [MSM 0021620860]; NASA;
Charles University [GAUK 280/2006/BGEO/MFF]
FX We thank Julie Castillo-Rogez for her comments during the course of this
study. G. Choblet, O. Grasset, G. Robuchon and G. Tobie benefited from
ANR ETHER and PNP-INSU in France. O. Cadek benefited from Charles
University Grant GAUK 280/2006/BGEO/MFF as well as the research project
MSM 0021620860 of the Ministry of Education in the Czech Republic. Part
of the work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology under a contract from NASA.
NR 69
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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 JUN
PY 2010
VL 207
IS 2
BP 959
EP 971
DI 10.1016/j.icarus.2009.12.002
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900040
ER
PT J
AU Anderson, RC
Beegle, LW
Peters, GH
Fleming, GM
Jandura, L
Kriechbaum, K
Manatt, K
Okon, A
Pounders, E
Sollitt, L
Sunshine, D
AF Anderson, Robert C.
Beegle, Luther W.
Peters, Gregory H.
Fleming, Gerald M., II
Jandura, Louise
Kriechbaum, Kristo
Manatt, Kenneth
Okon, Avi
Pounders, Erik
Sollitt, Luke
Sunshine, Dan
TI Particle transport and distribution on the Mars Science Laboratory
Mission: Effects of triboelectric charging (vol 204, pg 545, 2009)
SO ICARUS
LA English
DT Correction
C1 [Anderson, Robert C.; Beegle, Luther W.; Peters, Gregory H.; Fleming, Gerald M., II; Jandura, Louise; Kriechbaum, Kristo; Manatt, Kenneth; Okon, Avi; Pounders, Erik; Sunshine, Dan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sollitt, Luke] Northrop Grumman Aeronaut Syst, Sensors & Instruments Dept, Redondo Beach, CA 90278 USA.
RP Beegle, LW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Luther.Beegle@jpl.nasa.gov
NR 3
TC 0
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U1 1
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 JUN
PY 2010
VL 207
IS 2
BP 1013
EP 1013
DI 10.1016/j.icarus.2010.03.018
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 597VS
UT WOS:000277790900044
ER
PT J
AU Darr, S
Ricks, W
Lemos, KA
AF Darr, Stephen
Ricks, Wendell
Lemos, Katherine A.
TI Safer Systems: A NextGen Aviation Safety Strategic Goal
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
ID AUTOMATION
AB The Joint Planning and Development Office (JPDO), is charged by Congress with developing the concepts and plans for the Next Generation Air Transportation System (NextGen) [1]. The National Aviation Safety Strategic Plan (NASSP), developed by the Safety Working Group of the JPDO, focuses on establishing the goals, objectives, and strategies needed to realize the safety objectives of the NextGen Integrated Plan.
The three goals of the NASSP are Safer Practices, Safer Systems, and Safer Worldwide. Safer Practices emphasizes an integrated systematic approach to safety risk management through implementation of formalized Safety Management Systems (SMS) that incorporate safety data analysis processes, and the enhancement of methods for ensuring safety an inherent characteristic of NextGen. Safer Systems emphasizes implementation of safety-enhancing technologies, which will improve safety for human-centered interfaces and enhance the safety of airborne and ground-based systems. Safer Worldwide encourages coordinating the adoption of the safer practices and safer systems technologies, policies, and procedures worldwide, such that the maximum level of safety is achieved across air transportation system boundaries.
This introduces the NASSP and its development, and focuses on the Safer Systems elements of the NASSP, which incorporates three objectives for NextGen systems: 1) provide risk reducing system interfaces; 2) provide safety enhancements for airborne systems; and 3) provide safety enhancements for ground-based systems. Our goal is to expose avionics and air traffic management system developers to NASSP objectives and Safer Systems strategies.
C1 [Darr, Stephen] Dynam Aerosp Inc, Sharon, MA USA.
[Ricks, Wendell; Lemos, Katherine A.] NASA, Hampton, VA USA.
RP Darr, S (reprint author), Dynam Aerosp Inc, Sharon, MA USA.
NR 11
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U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD JUN
PY 2010
VL 25
IS 6
BP 9
EP 14
PG 6
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 663PE
UT WOS:000282899000002
ER
PT J
AU Del Castillo, L
Moussessian, A
McPherson, R
Zhang, T
Hou, ZW
Dean, R
Johnson, RW
AF Del Castillo, Linda
Moussessian, Alina
McPherson, Ryan
Zhang, Tan
Hou, Zhenwei
Dean, Robert
Johnson, R. Wayne
TI Flexible Electronic Assemblies for Space Applications
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
AB This describes the development and evaluation of advanced technologies for the integration of electronic devices within membrane polymers. Specifically, investigators thinned silicon die, electrically connecting them with circuits on flexible (liquid crystal polymer (LCP) and polyimide (PI) circuits, using gold thermo-compression flip chip bonding, and embedding them within the material. The influence of temperature and flexure on the electrical behavior of active embedded assemblies was evaluated. In addition, the long-term thermal cycle resistance of the passive daisy chain assemblies was determined within the Mil-Std (-55 degrees to +125 degrees C), extreme low #1 (-125 degrees to +85 degrees C), and extreme low #2 (-125 degrees to +125 degrees C) temperature ranges. The results of these evaluations will be discussed, along with the application of this technology for future NASA missions.
C1 [Del Castillo, Linda; Moussessian, Alina] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McPherson, Ryan; Zhang, Tan; Hou, Zhenwei; Dean, Robert; Johnson, R. Wayne] Auburn Univ, Auburn, AL 36849 USA.
RP Del Castillo, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 4
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U1 0
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD JUN
PY 2010
VL 25
IS 6
BP 25
EP 29
PG 5
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 663PE
UT WOS:000282899000005
ER
PT J
AU Campbell, JR
Reid, JS
Westphal, DL
Zhang, JL
Hyer, EJ
Welton, EJ
AF Campbell, James R.
Reid, Jeffrey S.
Westphal, Douglas L.
Zhang, Jianglong
Hyer, Edward J.
Welton, Ellsworth J.
TI CALIOP Aerosol Subset Processing for Global Aerosol Transport Model Data
Assimilation
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aerosols; laser radar; modeling; satellite applications
AB A system for processing Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) satellite-based 0.532 and 1.064 mu m elastic and polarization lidar datasets for global aerosol transport model assimilation is described. A method for constructing one-degree along-track and cloud-free signal composite averages, consistent with Navy Aerosol Analysis and Prediction System (NAAPS) model gridding, using CALIOP Level 1B attenuated backscatter and Level 2 cloud boundary-height products is outlined. Optimal vertical resolutions and relative signal uncertainties for the composite signal averages are described for both day and nighttime measurement scenarios. Depolarization profiles are described for the 0.532 mu m channel as well as attenuated color ratio profiles using 0.532 and 1.064 mu m attenuated backscatter measurements. Constrained by NAAPS model aerosol optical depths, processed attenuated backscatter profiles are inverted to solve for extinction and backscatter coefficients, their ratio, and extinction coefficient profiles which serve as the basis for data assimilation.
C1 [Campbell, James R.; Hyer, Edward J.] USN, Res Lab, Univ Corp, Atmospher Res Visiting Scientist Programs, Monterey, CA 93943 USA.
[Zhang, Jianglong] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Welton, Ellsworth J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Campbell, JR (reprint author), USN, Res Lab, Univ Corp, Atmospher Res Visiting Scientist Programs, Monterey, CA 93943 USA.
EM jamesc@ucar.edu; jeffrey.reid@nrlmry.navy.mil;
dou-glas.westphal@nrlmry.navy.mil; jzhang@aero.und.edu; ehyer@ucar.edu;
Ellsworth.J.Welton@nasa.gov
RI Hyer, Edward/E-7734-2011; Welton, Ellsworth/A-8362-2012; Campbell,
James/C-4884-2012; Reid, Jeffrey/B-7633-2014
OI Hyer, Edward/0000-0001-8636-2026; Campbell, James/0000-0003-0251-4550;
Reid, Jeffrey/0000-0002-5147-7955
FU National Aeronautics and Space Administration [NNH07AG441]; Office of
Naval Research [32, 35]
FX Manuscript received April 06, 2009; revised September 09, 2009; accepted
December 15, 2009. Current version published May 19, 2010. This work was
supported by the National Aeronautics and Space Administration under
Grant NNH07AG441 and by the Office of Naval Research Codes 32 and 35.
NR 0
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U1 0
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD JUN
PY 2010
VL 3
IS 2
BP 203
EP 214
DI 10.1109/JSTARS.2010.2044868
PG 12
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 599DJ
UT WOS:000277890100005
ER
PT J
AU Llombart, N
Cooper, KB
Dengler, RJ
Bryllert, T
Siegel, PH
AF Llombart, Nuria
Cooper, Ken B.
Dengler, Robert J.
Bryllert, Tomas
Siegel, Peter H.
TI Confocal Ellipsoidal Reflector System for a Mechanically Scanned Active
Terahertz Imager
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Reflector antennas; scanning antennas; submillimeter-wavelength imaging;
terahertz radar; THz
ID GREGORIAN ANTENNAS; ARRAY
AB We present the design of a reflector system that can rapidly scan and refocus a terahertz beam for high-resolution standoff imaging applications. The proposed optical system utilizes a confocal Gregorian geometry with a small mechanical rotating mirror and an axial displacement of the feed. For operation at submillimeter wavelengths and standoff ranges of many meters, the imaging targets are electrically very close to the antenna aperture. Therefore the main reflector surface must be an ellipse, instead of a parabola, in order to achieve the best imaging performance. Here we demonstrate how a simple design equivalence can be used to generalize the design of a Gregorian reflector system based on a paraboloidal main reflector to one with an ellipsoidal main reflector. The system parameters are determined by minimizing the optical path length error, and the results are validated with numerical simulations from the commercial antenna software package GRASP. The system is able to scan the beam over 0.5 m in cross-range at a 25 m standoff range with less than 1% increase of the half-power beam-width.
C1 [Llombart, Nuria; Cooper, Ken B.; Dengler, Robert J.; Bryllert, Tomas; Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bryllert, Tomas] Wasa Millimeter Wave AB, S-42341 Torslanda, Sweden.
[Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
RP Llombart, N (reprint author), Univ Complutense Madrid, Opt Dept, E-28040 Madrid, Spain.
EM nuria.llombart@opt.ucm.es; phs@caltech.edu
FU National Aeronautics and Space Administration; Naval Explosive Ordnance
Disposal Technology Division; DoD Physical Security Equipment Action
Group (PSEAG)
FX Manuscript received July 01, 2009; revised November 16, 2009; accepted
December 25, 2009. Date of publication March 29, 2010; date of current
version June 03, 2010. This work was carried out by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. This work was
supported under a contract to the California Institute of Technology,
Division of Biology, by the Naval Explosive Ordnance Disposal Technology
Division, with funding provided by the DoD Physical Security Equipment
Action Group (PSEAG).
NR 26
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD JUN
PY 2010
VL 58
IS 6
BP 1834
EP 1841
DI 10.1109/TAP.2010.2046860
PG 8
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 607UF
UT WOS:000278531600001
ER
PT J
AU Pogorzelski, RJ
AF Pogorzelski, Ronald J.
TI Experimental Demonstration of the Extended Probe Instrument Calibration
(EPIC) Technique
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Anechoic chambers (electromagnetic); antenna measurements; near-field
far-field transformation
AB A chamber calibration technique for spherical near-field antenna measurements proposed by Pogorzelski is experimentally demonstrated. The chamber was purposely degraded by introducing a metal plate situated so as to produce a strong specular reflection from the antenna under test to the chamber probe. The effects of this artifact were easily observed in the raw data. The chamber with the artifact was calibrated using an open ended waveguide calibration antenna and the resulting calibration coefficients were used to correct the raw measurement producing a result very similar to the measurement carried out in the undegraded chamber over about 30 to 35 dB of dynamic range.
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 pogo@ieee.org
NR 2
TC 4
Z9 4
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD JUN
PY 2010
VL 58
IS 6
BP 2093
EP 2097
DI 10.1109/TAP.2010.2048868
PG 5
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 607UF
UT WOS:000278531600030
ER
PT J
AU Kashyap, AS
Mantooth, HA
Vo, TA
Mojarradi, M
AF Kashyap, Avinash S.
Mantooth, H. Alan
Vo, Tuan A.
Mojarradi, Mohammad
TI Compact Modeling of LDMOS Transistors for Extreme Environment Analog
Circuit Design
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE Cryogenic; extreme environment; high-voltage (HV) MOSFET; impurity
freeze-out; laterally diffused MOS (LDMOS); MOS Model 20 (MM20)
ID QUASI-SATURATION; MOSFETS; TEMPERATURES; IONIZATION
AB The cryogenic characterization (93 K/-180 degrees C to 300 K/27 degrees C) and compact modeling of a high-voltage (HV) laterally diffused MOS (LDMOS) transistor that exhibits carrier freeze-out are presented in this paper. Unlike low-voltage MOS devices, it was observed that HVMOS structures experience freeze-out effects at much higher temperatures, resulting in an output current roll-off beyond a transition temperature. Standard compact models generally do not guarantee performance below 218 K (-55 degrees C), and freeze-out effects are certainly not incorporated in them. This causes the models to fail to track at lower temperatures, and designers relying on these models would be misled. In this paper, the temperature-scaling equations of the MOS Model 20 LDMOS model are modified to reflect the device operation down to 93 K, which is sufficient for designing sensor interface circuitry for lunar applications. The model is then validated against an LDMOS device designed by engineers at the Jet Propulsion Laboratory, using the IBM SiGe 5AM process. A modified parameter extraction procedure has also been developed. This generalized approach is compact model friendly and can also be implemented for other standard models. Analog circuits designed with this new model are currently being tested at the International Space Station.
C1 [Kashyap, Avinash S.; Mantooth, H. Alan] Univ Arkansas, Fayetteville, AR 72701 USA.
[Vo, Tuan A.; Mojarradi, Mohammad] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Kashyap, AS (reprint author), Gen Elect Global Res Ctr, Niskayuna, NY 12309 USA.
EM avi.kash@gmail.com; mantooth@uark.edu; tuan.a.vo@jpl.nasa.gov;
mohammad.m.mojarradi@jpl.nasa.gov
FU National Aeronautics and Space Administration [NNL05AA37C]; Jet
Propulsion Laboratory; IBM SiGe
FX Manuscript received October 15, 2009; revised March 1, 2010; accepted
March 5, 2010. Date of publication April 15, 2010; date of current
version May 19, 2010. This work was supported by the National
Aeronautics and Space Administration under Grant NNL05AA37C. The review
of this paper was arranged by Editor M. A. Shibib.; The authors would
like to thank C. Moore, A. Keyes, M. Watson, M. Beatty, L. Nadeau of the
National Aeronautics and Space Administration, E. Kolawa of the Jet
Propulsion Laboratory, and the IBM SiGe development group for their
support and the SiGe ETDP team for the many contributions, including B.
Blalock, W. Johnson, R. Garbos, R. Berger, F. Dai, G. Niu, L. Peltz, P.
McCluskey, M. Alles, R. Reed, A. Joseph, C. Eckert, J. Holmes, and J. D.
Cressler. The authors would also like to thank NXP Semiconductors for
providing the Verilog-A code of the MM20 model and Lynguent for
providing ModLyng.
NR 18
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U1 0
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD JUN
PY 2010
VL 57
IS 6
BP 1431
EP 1439
DI 10.1109/TED.2010.2046073
PG 9
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 599BD
UT WOS:000277884100031
ER
PT J
AU Huang, SW
Tsang, L
Njoku, EG
Chan, KS
AF Huang, Shaowu
Tsang, Leung
Njoku, Eni G.
Chan, Kuan Shan
TI Backscattering Coefficients, Coherent Reflectivities, and Emissivities
of Randomly Rough Soil Surfaces at L-Band for SMAP Applications Based on
Numerical Solutions of Maxwell Equations in Three-Dimensional
Simulations
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Microwave remote sensing; soil moisture; random rough surface; NMM3D
ID MONTE-CARLO SIMULATIONS; BOUNDARY-CONDITION METHOD; SCATTERING;
ENHANCEMENT; MOISTURE; WAVES
AB We used Numerical Maxwell Model in 3-D Simulations (NMM3D) to study the backscattering coefficients, coherent reflectivities, and emissivities of soil surfaces using Gaussian random rough surfaces with exponential correlation functions. The surface area used is 8 by 8 square wavelengths. A total of close to 200 cases are computed by varying rms height, correlation length, and soil permittivity. We consider a 40 degrees incidence angle. For each case, 15 realizations of rough surface profiles are generated, and 30 solutions of Maxwell equations are computed because of two polarizations. The method for solving the Maxwell equations is based on the Method of Moments (MoM) with Rao-Wilton-Glisson (RWG) basis functions. The solutions are accelerated by the sparse matrix canonical grid method implemented on parallel computing. The rms height varies up to 0.126 wavelength. The results are compared with the Dubois formulation, Small Perturbation Method (SPM), Kirchhoff Approximation (KA), and Advanced Integral Equation Model (AIEM). The NMM3D results are also compared with VV and HH backscatter data of soil surfaces where ground truth rms heights and correlation lengths were both measured. Good agreement is found between the NMM3D results and experimental measurement data. Based on the computed cases, interpolation tables are derived that can be directly applied to L-band active and passive microwave remote sensing of soil moisture, such as for the upcoming Soil Moisture Active and Passive (SMAP) mission.
C1 [Huang, Shaowu; Tsang, Leung] Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA.
[Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chan, Kuan Shan] Natl Cent Univ, Ctr Space & Remote Sensing Res, Chungli 32054, Taiwan.
RP Huang, SW (reprint author), Univ Washington, Dept Elect Engn, Seattle, WA 98195 USA.
EM tsang@ee.washington.edu
FU National Aeronautics and Space Administration's Soil Moisture Active and
Passive mission
FX Manuscript received October 18, 2009; revised December 22, 2009. Date of
publication March 18, 2010; date of current version May 19, 2010. This
work was supported by the National Aeronautics and Space
Administration's Soil Moisture Active and Passive mission.
NR 24
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U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JUN
PY 2010
VL 48
IS 6
BP 2557
EP 2568
DI 10.1109/TGRS.2010.2040748
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 597PY
UT WOS:000277772200010
ER
PT J
AU Larsen, KW
Jurgens, RF
Haldemann, AFC
Slade, MA
Rumsey, HC
AF Larsen, Kristopher W.
Jurgens, Raymond F.
Haldemann, Albert F. C.
Slade, Martin A.
Rumsey, Howard C., Jr.
TI Terrestrial Quadstatic Interferometric Radar Observations of Mars
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Planets; radar data processing; radio interferometry; remote sensing
ID MARTIAN TOPOGRAPHY; SURFACE-PROPERTIES; LUNAR TOPOGRAPHY; VENUS;
EXPLORATION; LOCALIZATION; BRIGHTNESS; SCATTERING; IMAGES; TITAN
AB A new technique for resolving the ambiguity inherent in delay-Doppler radar observations of Mars has been developed and implemented using a suite of data collected during 2001, 2003, and 2005 oppositions. New recording systems, processing techniques, and, most importantly, the addition of a fourth receiving telescope allow for the high-resolution mapping of Mars' radar properties. In this paper, we develop a maximum likelihood method to probabilistically estimate the contributions to the received radar signal from the ambiguous resolution cells. Our delay-Doppler interferometric radar observations are designed to map the radar properties of Mars surface while disregarding the historically typical goal of measuring topography, instead using Mars' topography as a priori knowledge. Example data from the September 27, 2003 observation over Mars' southern highlands, including Ma'adim Vallis and Gusev Crater, and the June 7, 2001 observation crossing Terra Meridiani are presented to demonstrate the effectiveness of the technique. Analysis of these observations predicted a root-mean-square ( rms) roughness, or slopes, for the Mars Exploration Rover ( MER) Spirit landing site of 1.80 degrees +/- 0.75 degrees. Similarly, analysis of the Gusev Crater landing site of MER Opportunity predicted rms slopes of 1.1 degrees +/- 0.1 degrees. Both predictions were validated by analysis of in situ rover images.
C1 [Larsen, Kristopher W.; Jurgens, Raymond F.; Haldemann, Albert F. C.; Slade, Martin A.; Rumsey, Howard C., Jr.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Larsen, KW (reprint author), Amer Phys Soc, Washington, DC 20004 USA.
EM Larsen.Kristopher@gmail.com
NR 47
TC 1
Z9 1
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JUN
PY 2010
VL 48
IS 6
BP 2670
EP 2684
DI 10.1109/TGRS.2010.2040084
PG 15
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 597PY
UT WOS:000277772200020
ER
PT J
AU Skuza, JR
Clavero, C
Yang, K
Wincheski, B
Lukaszew, RA
AF Skuza, J. R.
Clavero, C.
Yang, K.
Wincheski, B.
Lukaszew, R. A.
TI Microstructural, Magnetic Anisotropy, and Magnetic Domain Structure
Correlations in Epitaxial FePd Thin Films With Perpendicular Magnetic
Anisotropy
SO IEEE TRANSACTIONS ON MAGNETICS
LA English
DT Article
DE Magnetic domains; perpendicular magnetic anisotropy (PMA); perpendicular
magnetic recording; thin films
ID CHEMICAL ORDER; STRAIN RELAXATION; LAYER THICKNESS; GROWTH
AB L1(0) order was optimized in FePd epitaxial thin films prepared using dc magnetron sputter deposition on MgO(001) substrates by investigating various growth temperatures. A series of films was grown at the optimal temperature with varying thickness and degree of chemical order to investigate the interplay between the microstructure, magnetic anisotropy, and magnetic domain structure. The experimentally measured magnetic domain size/period and magnetic anisotropy in this high perpendicular anisotropy system were found to be correlated following the analytical energy model proposed by Kooy and Enz that considers a delicate balance between the domain wall energy and the demagnetizing stray field energy.
C1 [Skuza, J. R.; Lukaszew, R. A.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Clavero, C.; Yang, K.; Lukaszew, R. A.] Coll William & Mary, Dept Appl Sci, Williamsburg, VA 23187 USA.
[Wincheski, B.] NASA, Nondestruct Evaluat Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Skuza, JR (reprint author), Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
EM jrskuza@wm.edu
RI Skuza, Jonathan/E-9048-2010; Clavero, Cesar/C-4391-2008; Yang,
Kaida/K-7916-2012
OI Skuza, Jonathan/0000-0002-9252-2708; Clavero, Cesar/0000-0001-6665-3141;
Yang, Kaida/0000-0003-2018-2625
FU Virginia Space Grant Consortium; National Science Foundation
[DMR-0355171]; Research Corporation; American Chemical Society
[PRF-41319-AC10]
FX The authors would like to thank K. Seo, J. Lu, and S. A. Wolf for
technical collaboration. This work was supported by the Virginia Space
Grant Consortium, National Science Foundation (DMR-0355171), Research
Corporation (Cottrell Scholar Award), and the American Chemical Society
(PRF-41319-AC10).
NR 24
TC 15
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U1 2
U2 29
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9464
J9 IEEE T MAGN
JI IEEE Trans. Magn.
PD JUN
PY 2010
VL 46
IS 6
BP 1886
EP 1889
DI 10.1109/TMAG.2009.2039923
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 601DH
UT WOS:000278037800159
ER
PT J
AU Fox, BP
Simmons-Potter, K
Thomes, WJ
Kliner, DAV
AF Fox, Brian P.
Simmons-Potter, Kelly
Thomes, William J., Jr.
Kliner, Dahv A. V.
TI Gamma-Radiation-Induced Photodarkening in Unpumped Optical Fibers Doped
With Rare-Earth Constituents
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Co-60; dose rate effects; passive irradiation; photodarkening;
radiation-induced absorption; rare-earth doped fibers; unpumped
amplifier
ID SILICA FIBERS; AMPLIFIERS; POWER; ENVIRONMENT; GLASSES; GAIN
AB Fibers doped with rare-earth constituents such as Er(3+) and Yb(3+) are exceedingly important to designers of fiber-optical systems due to their ability to amplify signals in the near infra-red, low-absorption regions of conventional silicate fibers. Extending the range of operating conditions for these systems to include adverse radiation environments requires a detailed study of the behavior of the fiber when subjected to relevant radiation fluxes of various cumulative doses and dose rates. Of particular interest in many applications is the effect of gamma radiation, which is known to degrade optical signal transmittance by creating absorption centers in the material. A study of radiation-induced photodarkening effect in unpumped Er(3), Yb(3+), and Er(3+)/Yb(3+) co-doped fibers under Co(60) gamma-irradiation is the focus of this paper. Specifically, the temporal evolution of the fiber transmittance in the near infra-red region from similar to 1.0 mu m-1.6 mu m was investigated, subjected to a multitude of exposure conditions spanning different dose-rates and total accumulated doses. The Er(3+)/Yb(3+) co-doped fiber was found to be the most radiation resistant, while the Er(3+) doped fiber was found to be the most radiation sensitive in this wavelength region. Dose rate and compositional dependencies were also observed in all fibers.
C1 [Fox, Brian P.; Simmons-Potter, Kelly] Univ Arizona, Tucson, AZ USA.
[Thomes, William J., Jr.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kliner, Dahv A. V.] JDS Uniphase Corp, Milpitas, CA 95035 USA.
RP Fox, BP (reprint author), Univ Arizona, Tucson, AZ USA.
EM kspotter@ece.arizona.edu
FU University of Arizona and the State of Arizona TRIF funds; Laboratory
Directed Research and Development, Sandia National Laboratories
[DE-AC04-94AL85000]
FX Manuscript received August 17, 2009; revised November 13, 2009; accepted
January 13, 2010. Date of current version June 16, 2010. This work was
supported jointly by the University of Arizona and the State of Arizona
TRIF funds and by Laboratory Directed Research and Development, Sandia
National Laboratories, under Contract DE-AC04-94AL85000.
NR 36
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U1 0
U2 13
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JUN
PY 2010
VL 57
IS 3
BP 1618
EP 1625
DI 10.1109/TNS.2010.2043854
PN 3
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 611JV
UT WOS:000278812300014
ER
PT J
AU De Geronimo, G
Rehak, P
Ackley, K
Carini, G
Chen, W
Fried, J
Keister, J
Li, SR
Li, Z
Pinelli, DA
Siddons, DP
Vernon, E
Gaskin, JA
Ramsey, BD
Tyson, TA
AF De Geronimo, Gianluigi
Rehak, Pavel
Ackley, Kim
Carini, Gabriella
Chen, Wei
Fried, Jack
Keister, Jeffrey
Li, Shaorui
Li, Zheng
Pinelli, Donald A.
Siddons, D. Peter
Vernon, Emerson
Gaskin, Jessica A.
Ramsey, Brian D.
Tyson, Trevor A.
TI ASIC for SDD-Based X-Ray Spectrometers
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE ASIC; charge sharing; high rate; LVDS; PUR; SDD
ID SILICON DRIFT DETECTORS; CHARGE-SENSITIVE PREAMPLIFIER; CMOS PEAK
DETECT; CONTINUOUS RESET; READOUT CIRCUIT; HOLD CIRCUITS; PULSE; JFET;
CONFIGURATION; SPECTROSCOPY
AB We present an application-specific integrated circuit (ASIC) for high-resolution x-ray spectrometers (XRS). The ASIC reads out signals from pixelated silicon drift detectors (SDDs). The pixel does not have an integrated field effect transistor (FET); rather, readout is accomplished by wire-bonding the anodes to the inputs of the ASIC. The ASIC dissipates 32 mW, and offers 16 channels of low-noise charge amplification, high-order shaping with baseline stabilization, discrimination, a novel pile-up rejector, and peak detection with an analog memory. The readout is sparse and based on custom low-power tristatable low-voltage differential signaling (LPT-LVDS). A unit of 64 SDD pixels, read out by four ASICs, covers an area of 12.8 cm(2) and dissipates with the sensor biased about 15 m W/cm(2). As a tile-based system, the 64-pixel units cover a large detection area. Our preliminary measurements at -44 degrees C show a FWHM of 145 eV at the 5.9 keV peak of a (55)Fe source, and less than 80 eV on a test-pulse line at 200 eV.
C1 [De Geronimo, Gianluigi; Rehak, Pavel; Ackley, Kim; Carini, Gabriella; Chen, Wei; Fried, Jack; Keister, Jeffrey; Li, Shaorui; Li, Zheng; Pinelli, Donald A.; Siddons, D. Peter; Vernon, Emerson] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Gaskin, Jessica A.; Ramsey, Brian D.] George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Tyson, Trevor A.] New Jersey Inst Technol, Newark, NJ 07102 USA.
RP De Geronimo, G (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM degeronimo@bnl.gov; rehak@bnl.gov; ackley@bnl.gov; carini@bnl.gov;
weichen@bnl.gov; jfried@bnl.gov; jkeister@bnl.gov; shaoruili@bnl.gov;
zhengl@bnl.gov; pinelli@bnl.gov; siddons@bnl.gov; evernon@bnl.gov;
jessica.gaskin@nasa.gov; brian.ramsey@nasa.gov; Tyson@adm.njit.edu
NR 43
TC 10
Z9 10
U1 1
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JUN
PY 2010
VL 57
IS 3
BP 1654
EP 1663
DI 10.1109/TNS.2010.2044809
PN 3
PG 10
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 611JV
UT WOS:000278812300019
ER
PT J
AU Simon, D
Simon, DL
AF Simon, Dan
Simon, Donald L.
TI Analytic Confusion Matrix Bounds for Fault Detection and Isolation Using
a Sum-of-Squared-Residuals Approach
SO IEEE TRANSACTIONS ON RELIABILITY
LA English
DT Article
DE Aircraft turbofan engine; chi-squared distribution; confusion matrix;
diagnosis probability matrix; fault detection and isolation
ID DIAGNOSIS; SUPERVISION; OBSERVERS; ACTUATOR; SYSTEMS
AB Given a system which can fail in 1 of n different ways, a fault detection and isolation (FDI) algorithm uses sensor data to determine which fault is the most likely to have occurred. The effectiveness of an FDI algorithm can be quantified by a confusion matrix, also called a diagnosis probability matrix, which indicates the probability that each fault is isolated given that each fault has occurred. Confusion matrices are often generated with simulation data, particularly for complex systems. In this paper, we perform FDI using sum-of-squared residuals (SSRs). We assume that the sensor residuals are s-independent and Gaussian, which gives the SSRs chi-squared distributions. We then generate analytic lower, and upper bounds on the confusion matrix elements. This approach allows for the generation of optimal sensor sets without numerical simulations. The confusion matrix bounds are verified with simulated aircraft engine data.
C1 [Simon, Dan] Cleveland State Univ, Dept Elect & Comp Engn, Cleveland, OH 44115 USA.
[Simon, Donald L.] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Simon, D (reprint author), Cleveland State Univ, Dept Elect & Comp Engn, Cleveland, OH 44115 USA.
EM d.j.simon@csuohio.edu; donald.l.simon@grc.nasa.gov
FU NASA
FX Manuscript received April 05, 2009; revised July 08, 2009, September 04,
2009, and October 16, 2009; accepted October 26, 2009. Date of
publication-April 19, 2010; date of current version June 03, 2010. This
work was supported by the NASA Faculty Fellowship Program. Associate
Editor: H. Li.
NR 28
TC 5
Z9 5
U1 0
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9529
J9 IEEE T RELIAB
JI IEEE Trans. Reliab.
PD JUN
PY 2010
VL 59
IS 2
BP 287
EP 296
DI 10.1109/TR.2010.2046772
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Software
Engineering; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA 607VO
UT WOS:000278535600003
ER
PT J
AU Blackmore, L
Ono, M
Bektassov, A
Williams, BC
AF Blackmore, Lars
Ono, Masahiro
Bektassov, Askar
Williams, Brian C.
TI A Probabilistic Particle-Control Approximation of Chance-Constrained
Stochastic Predictive Control
SO IEEE TRANSACTIONS ON ROBOTICS
LA English
DT Article
DE Chance constraints; hybrid discrete-continuous systems; nonholonomic
motion planning; planning under stochastic uncertainty
ID MARKOV LINEAR-SYSTEMS; ROBUST-CONTROL
AB Robotic systems need to be able to plan control actions that are robust to the inherent uncertainty in the real world. This uncertainty arises due to uncertain state estimation, disturbances, and modeling errors, as well as stochastic mode transitions such as component failures. Chance-constrained control takes into account uncertainty to ensure that the probability of failure, due to collision with obstacles, for example, is below a given threshold. In this paper, we present a novel method for chance-constrained predictive stochastic control of dynamic systems. The method approximates the distribution of the system state using a finite number of particles. By expressing these particles in terms of the control variables, we are able to approximate the original stochastic control problem as a deterministic one; furthermore, the approximation becomes exact as the number of particles tends to infinity. This method applies to arbitrary noise distributions, and for systems with linear or jump Markov linear dynamics, we show that the approximate problem can be solved using efficient mixed-integer linear-programming techniques. We also introduce an important weighting extension that enables the method to deal with low-probability mode transitions such as failures. We demonstrate in simulation that the new method is able to control an aircraft in turbulence and can control a ground vehicle while being robust to brake failures.
C1 [Blackmore, Lars] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ono, Masahiro; Williams, Brian C.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
[Bektassov, Askar] Eni E&P, I-00144 Rome, Italy.
RP Blackmore, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM lars@jpl.nasa.gov; hiro_ono@mit.edu; askar.bektassov@gmail.com;
williams@mit.edu
FU National Aeronautics and Space Administration (NASA) [NNA04CK91A]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) under the NASA Award NNA04CK91A.
NR 57
TC 84
Z9 87
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1552-3098
J9 IEEE T ROBOT
JI IEEE Trans. Robot.
PD JUN
PY 2010
VL 26
IS 3
BP 502
EP 517
DI 10.1109/TRO.2010.2044948
PG 16
WC Robotics
SC Robotics
GA 607XW
UT WOS:000278541600008
ER
PT J
AU Giannakopoulou, D
Pasareanu, CS
AF Giannakopoulou, Dimitra
Pasareanu, Corina S.
TI Automated Compositional Verification
SO IET SOFTWARE
LA English
DT Editorial Material
C1 [Giannakopoulou, Dimitra; Pasareanu, Corina S.] NASA, Ames Res Ctr, Robust Software Engn Grp, Washington, DC 20546 USA.
[Pasareanu, Corina S.] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
RP Giannakopoulou, D (reprint author), NASA, Ames Res Ctr, Robust Software Engn Grp, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU INST ENGINEERING TECHNOLOGY-IET
PI HERTFORD
PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD SG1 2AY, ENGLAND
SN 1751-8806
J9 IET SOFTW
JI IET Softw.
PD JUN
PY 2010
VL 4
IS 3
BP 179
EP 180
DI 10.1049/iet-sen.2010.9053
PG 2
WC Computer Science, Software Engineering
SC Computer Science
GA 617CO
UT WOS:000279258600001
ER
PT J
AU Nishikawa, KI
Nimiec, J
Medvedev, M
Zhang, B
Hardee, P
Mizuno, Y
Nordlund, A
Frederiksen, J
Sol, H
Pohl, M
Hartmann, DH
Oka, M
Fishman, JF
AF Nishikawa, K. -I.
Nimiec, J.
Medvedev, M.
Zhang, B.
Hardee, P.
Mizuno, Y.
Nordlund, A.
Frederiksen, J.
Sol, H.
Pohl, M.
Hartmann, D. H.
Oka, M.
Fishman, J. F.
TI RADIATION FROM RELATIVISTIC SHOCKS WITH TURBULENT MAGNETIC FIELDS
SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D
LA English
DT Article; Proceedings Paper
CT International Meeting on High-Energy Phenomena in Relativistic Outflows
II
CY OCT 26-30, 2009
CL Burnod Aires, ARGENTINA
DE Weibel instability; particle acceleration; radiation
ID RAY BURST SOURCES; PARTICLE-ACCELERATION; COLLISIONLESS SHOCKS; WEIBEL
INSTABILITY; PROMPT EMISSION; PLASMA; GENERATION; EVOLUTION
AB Using our new 3D relativistic electromagnetic particle (REMP) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron-positron jet propagating in an unmagnetized ambient electron-positron plasma. We have also performed simulations with electron-ion jets. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability for electron-positron jets and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks for pair plasma case. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value for pair plasmas. Behind the bow shock in the jet shock strong electromagnetic fields are generated. These fields may lead to time-dependent afterglow emission. We calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We also used the new technique to calculate emission from electrons based on simulations with a small system with two different cases for Lorentz factors (15 and 100). We obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability.
C1 [Nishikawa, K. -I.; Mizuno, Y.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Nimiec, J.] Inst Nucl Phys PAN, PL-31342 Krakow, Poland.
[Medvedev, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Zhang, B.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Nordlund, A.; Frederiksen, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Sol, H.] Observ Paris, LUTH, F-92195 Meudon, France.
[Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Oka, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fishman, J. F.] NASA, MSFC, Huntsville, AL 35805 USA.
RP Nishikawa, KI (reprint author), Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
RI Nordlund, Aake/M-4528-2014; Frederiksen, Jacob Trier/P-6757-2015;
Mizuno, Yosuke/D-5656-2017
OI Nordlund, Aake/0000-0002-2219-0541; Frederiksen, Jacob
Trier/0000-0002-3560-0044; Mizuno, Yosuke/0000-0002-8131-6730
NR 26
TC 7
Z9 7
U1 0
U2 4
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0218-2718
J9 INT J MOD PHYS D
JI Int. J. Mod. Phys. D
PD JUN
PY 2010
VL 19
IS 6
BP 715
EP 721
DI 10.1142/S0218271810016865
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 615MU
UT WOS:000279140200012
ER
PT J
AU Gehrels, N
Cannizzo, JK
AF Gehrels, N.
Cannizzo, J. K.
TI GAMMA-RAY BURSTS - OBSERVATIONS
SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D
LA English
DT Article; Proceedings Paper
CT International Meeting on High-Energy Phenomena in Relativistic Outflows
II
CY OCT 26-30, 2009
CL Burnod Aires, ARGENTINA
ID 28 FEBRUARY 1997; HOST GALAXY; AFTERGLOW; GRB-050709; EMISSION;
REDSHIFT; SUPERNOVAE; TELESCOPE; DISCOVERY; ORIGIN
AB We are in an exciting period of discovery for gamma-ray bursts. The Swift observatory is detecting 100 bursts per year, providing arcsecond localizations and sensitive observations of the prompt and afterglow emission. The Fermi observatory is observing 250 bursts per year with its medium-energy GRB instrument and about 10 bursts per year with its high-energy LAT instrument. In addition, rapid-response telescopes on the ground are providing new capabilities to study optical emission during the prompt phase and spectral signatures of the host galaxies. The combined data set is enabling great advances in our understanding of GRBs including afterglow physics, short burst origin, and high-energy emission.
C1 [Gehrels, N.; Cannizzo, J. K.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, CRESST,UMBC, Greenbelt, MD 20771 USA.
RP Gehrels, N (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, CRESST,UMBC, Greenbelt, MD 20771 USA.
EM neil.gehrels@nasa.gov; john.k.cannizzo@nasa.gov
RI Gehrels, Neil/D-2971-2012
NR 33
TC 0
Z9 0
U1 0
U2 1
PU WORLD SCIENTIFIC PUBL CO PTE LTD
PI SINGAPORE
PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE
SN 0218-2718
J9 INT J MOD PHYS D
JI Int. J. Mod. Phys. D
PD JUN
PY 2010
VL 19
IS 6
BP 977
EP 984
DI 10.1142/S021827181001710X
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 615MU
UT WOS:000279140200047
ER
PT J
AU Ponomarev, AL
Huff, J
Cucinotta, FA
AF Ponomarev, Artem L.
Huff, Janice
Cucinotta, Francis A.
TI The analysis of the densely populated patterns of radiation-induced foci
by a stochastic, Monte Carlo model of DNA double-strand breaks induction
by heavy ions
SO INTERNATIONAL JOURNAL OF RADIATION BIOLOGY
LA English
DT Article
DE radiation of human cells; DNA damage foci; DSB; NASA Radiation Track
Image model; image segmentation; Monte Carlo method
ID HISTONE H2AX PHOSPHORYLATION; GAMMA-H2AX FOCI; IONIZING-RADIATION;
PARTICLE RADIATION; EXPOSURE; REPAIR; CELLS; RAYS; DISTRIBUTIONS;
VOLUMES
AB Purpose: To resolve the difficulty in counting merged DNA damage foci in high-LET (linear energy transfer) ion-induced patterns.
Materials and methods: The analysis of patterns of RIF (radiation-induced foci) produced by high-LET Fe and Ti ions were conducted by using a Monte Carlo model that combines the heavy ion track structure with characteristics of the human genome on the level of chromosomes. The foci patterns were also simulated in the maximum projection plane for flat nuclei.
Results: The model predicts the spatial and genomic distributions of DNA DSB (double-strand breaks) in a cell nucleus for a particular dose of radiation. We used the model to do analyses for three irradiation scenarios: (i) The ions were oriented perpendicular to the flattened nuclei in a cell culture monolayer; (ii) the ions were parallel to that plane; and (iii) round nucleus. In the parallel scenario we found that the foci appeared to be merged due to their high density, while, in the perpendicular scenario, the foci appeared as one bright spot per hit. The statistics and spatial distribution of regions of densely arranged foci, termed DNA foci chains, were predicted numerically using this model. Another analysis was done to evaluate the number of ion hits per nucleus, which were visible from streaks of closely located foci.
Conclusions: We showed that DSB clustering needs to be taken into account to determine the true DNA damage foci yield, which helps to determine the DSB yield. Using the model analysis, a researcher can refine the DSB yield per nucleus per particle. We showed that purely geometric artifacts, present in the experimental images, can be analytically resolved with the model, and that the quantisation of track hits and DSB yields can be provided to the experimentalists who use enumeration of radiation-induced foci in immunofluorescence experiment using proteins that detect DNA damage.
C1 [Ponomarev, Artem L.; Huff, Janice; Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Ponomarev, Artem L.; Huff, Janice] Univ Space Res Assoc, Houston, TX USA.
RP Ponomarev, AL (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code SK,2101 NASA Pkwy,Bldg 37,119, Houston, TX 77058 USA.
EM artem.l.ponomarev@nasa.gov
FU NASA [DE-AIO2-09ER64843]
FX The simulations were done on the NASA JSC Beowulf cluster machine.
Funding was through the NASA Risk Assessment Project, #DE-AIO2-09ER64843
NR 19
TC 10
Z9 10
U1 2
U2 5
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0955-3002
J9 INT J RADIAT BIOL
JI Int. J. Radiat. Biol.
PD JUN
PY 2010
VL 86
IS 6
BP 507
EP 515
DI 10.3109/09553001003717175
PG 9
WC Biology; Nuclear Science & Technology; Radiology, Nuclear Medicine &
Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Nuclear Science &
Technology; Radiology, Nuclear Medicine & Medical Imaging
GA 620EO
UT WOS:000279482000009
PM 20470200
ER
PT J
AU de los Rios, A
Valea, S
Ascaso, C
Davila, A
Kastovsky, J
Mckay, CP
Gomez-Silva, B
Wierzchos, J
AF de los Rios, Asuncion
Valea, Sergio
Ascaso, Carmen
Davila, Alfonso
Kastovsky, Jan
Mckay, Christopher P.
Gomez-Silva, Benito
Wierzchos, Jacek
TI Comparative analysis of the microbial communities inhabiting halite
evaporites of the Atacama Desert
SO INTERNATIONAL MICROBIOLOGY
LA English
DT Article
DE Archaea; Bacteria; Cyanobacteria; prokaryotic diversity; halite
evaporites; Atacama Desert
ID PROKARYOTIC GENETIC DIVERSITY; MULTIPOND SOLAR SALTERN; NORTHERN CHILE;
HALOCOCCUS-SALIFODINAE; BACTERIAL DIVERSITY; SALINITY GRADIENT; ARCHAEAL
ISOLATE; SP-NOV.; CYANOBACTERIA; LIFE
AB Molecular biology and microscopy techniques were used to characterize the microbial communities inside halite evaporites from different parts of the Atacama Desert. Denaturing gradient gel electrophoresis (DGGE) analysis revealed that the evaporite rocks harbor communities predominantly made up of cyanobacteria, along with heterotrophic bacteria and archaea. Different DGGE profiles were obtained for the different sites, with the exception of the cyanobacterial profile, in which only one phylotype was detected across the three sites examined. Chroococcidiopsis-like cells were the only cyanobacterial components of the rock samples, although the phylogenetic study revealed their closer genetic affinity to Halothece genera. Gene sequences of the heterotrophic bacteria and archaea indicated their proximity to microorganisms found in other hypersaline environments. Microorganisms colonizing these halites formed microbial aggregates in the pore spaces between halite crystals, where microbial interactions occur. In this exceptional, salty, porous halite rock habitat, microbial consortia with a community structure probably conditioned by the environmental conditions occupy special microhabitats with physical and chemical properties that promote their survival. [Int Microbiol 2010; 13(2):79-89]
C1 [de los Rios, Asuncion; Valea, Sergio; Ascaso, Carmen; Wierzchos, Jacek] CSIC, CCMA, Inst Recursos Natur, Madrid 28006, Spain.
[Davila, Alfonso] SETI Inst, Mountain View, CA USA.
[Kastovsky, Jan] Univ S Bohemia, Fac Sci, Ceske Budejovice, Czech Republic.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gomez-Silva, Benito] Univ Antofagasta, Biochem Unit, Antofagasta, Chile.
RP de los Rios, A (reprint author), CSIC, CCMA, Inst Recursos Natur, 115 Bis, Madrid 28006, Spain.
EM arios@ccma.csic.es
RI Wierzchos, Jacek/F-7036-2011; Ascaso, Carmen/F-5369-2011; Davila,
Alfonso/A-2198-2013; de los Rios, Asuncion/L-3694-2014
OI Wierzchos, Jacek/0000-0003-3084-3837; Ascaso,
Carmen/0000-0001-9665-193X; Davila, Alfonso/0000-0002-0977-9909; de los
Rios, Asuncion/0000-0002-0266-3516
FU Spanish Ministry of Science and Innovation [CGL2007-62875/BOS,
CGL2006-04658, CTM2009-12838-CO4-O3]; CSIC, Spain [PIE-631A,
PIE-200630/184]
FX The authors thank Fernando Pinto and Maria J. Malo for their technical
assistance, Sergio Perez-Ortega for useful comments concerning the
phylogenetic analysis, and Ana Burton for revising the English. This
work was supported by grant CGL2007-62875/BOS, CGL2006-04658 and
CTM2009-12838-CO4-O3 from the Spanish Ministry of Science and Innovation
and grants PIE-631A and PIE-200630/184 from the CSIC, Spain.
NR 50
TC 40
Z9 40
U1 2
U2 39
PU VIGUERA EDITORES, S L
PI BARCELONA
PA PLAZA TETUAN, 7, BARCELONA, E-08010, SPAIN
SN 1139-6709
J9 INT MICROBIOL
JI Int. Microbiol.
PD JUN
PY 2010
VL 13
IS 2
BP 79
EP 89
DI 10.2436/20.1501.01.113
PG 11
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA 648PI
UT WOS:000281706000004
PM 20890842
ER
PT J
AU Han, M
Braun, SA
Olson, WS
Persson, POG
Bao, JW
AF Han, Mei
Braun, Scott A.
Olson, William S.
Persson, P. Ola G.
Bao, Jian-Wen
TI Application of TRMM PR and TMI Measurements to Assess Cloud
Microphysical Schemes in the MM5 for a Winter Storm
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID REMOTE-SENSING APPLICATIONS; MELTING-LAYER MODEL; PART II;
PRECIPITATION; SIMULATIONS; PARAMETERIZATION; SENSITIVITY; CONVECTION;
MESOSCALE; EVOLUTION
AB This paper uses observations from Tropical Rainfall Measuring Mission (TRMM) precipitation radar (PR) and microwave imager (TMI) to evaluate the cloud microphysical schemes in the fifth-generation Pennsylvania State University-National Center for Atmospheric Research Mesoscale Model (MM5; version 3.7.4) for a wintertime frontal precipitation system over the eastern Pacific Ocean. By incorporating a forward radiative transfer model, the radar reflectivity and brightness temperatures are simulated and compared with the observations at PR and TMI frequencies. The main purpose of this study is to identify key differences among the five schemes [including Simple ice, Reisner1, Reisner2, Schultz, and Goddard Space Flight Center (GSFC) microphysics scheme] in the MM5 that may lead to significant departures of simulated precipitation properties from both active (PR) and passive (TMI) microwave observations. Radiative properties, including radar reflectivity, attenuation, and scattering in precipitation liquid and ice layers are investigated. In the rain layer, most schemes are capable of reproducing the observed radiative properties to a reasonable degree; the Reisner2 simulation, however, produces weaker reflectivity and stronger attenuation than the observations, which is possibly attributable to the larger intercept parameter (N(0r)) applied in this run. In the precipitation ice layer, strong evidence regarding the differences in the microphysical and radiative properties between a narrow cold-frontal rainband (NCFR) and a wide cold-frontal rainband (WCFR) within this frontal precipitation system is found. The performances of these schemes vary significantly on simulating the microphysical and radiative properties of the frontal rainband. The GSFC scheme shows the least bias, while the Reisner1 scheme has the largest bias in the reflectivity comparison. It appears more challenging for the model to replicate the scattering signatures obtained by the passive sensor (TMI). Despite the common problem of excessive scattering in the WCFR (stratiform precipitation) region in every simulation, the magnitude of the scattering maximum seems better represented in the Reisner2 scheme. The different types of precipitation ice, snow, and graupel are found to behave differently in the relationship of scattering versus reflectivity. The determinative role of the precipitation ice particle size distribution (intercept parameters) is extensively discussed through sensitivity tests and a single-layer radiative transfer model.
C1 [Han, Mei] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA.
[Han, Mei; Braun, Scott A.; Olson, William S.] NASA, Mesoscale Atmospher Proc Branch, Atmospheres Lab, GSFC, Greenbelt, MD 20771 USA.
[Olson, William S.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA.
[Persson, P. Ola G.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Persson, P. Ola G.; Bao, Jian-Wen] NOAA, Earth Syst Res Lab, Boulder, CO USA.
RP Han, M (reprint author), NASA, Mesoscale Atmospher Proc Branch, Atmospheres Lab, GSFC, Code 613-1, Greenbelt, MD 20771 USA.
EM mei.han@nasa.gov
RI Han, Mei/H-2344-2012
FU NASA
FX The authors thank Dr. Paul Schultz at the NOAA/ESRL for his great help
on understanding the Schultz scheme in the MM5. The author is very
grateful for many beneficial discussions related to cloud modeling and
radar with Drs. Xiaowen Li, Lin Tian, Mircea Grecu, Steve Lang, and
Lihua Li at NASA/GSFC. Suggestions from Dr. Grant W. Petty at University
of Wisconsin-Madison in the early stage of this study are greatly
appreciated. The authors also gratefully acknowledge two anonymous
reviewers and Dr. Benjamin Johnson at NASA/GSFC for their very valuable
comments. This work was supported by Dr. Ramesh Kakar at NASA
Headquarters with funds from the NASA Precipitation Measurement Mission
science program.
NR 33
TC 7
Z9 7
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JUN
PY 2010
VL 49
IS 6
BP 1129
EP 1148
DI 10.1175/2010JAMC2327.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 634SC
UT WOS:000280604200005
ER
PT J
AU Komatsu, H
Hashimoto, H
Kume, T
Tanaka, N
Yoshifuji, N
Otsuki, K
Suzuki, M
Kumagai, T
AF Komatsu, Hikaru
Hashimoto, Hirofumi
Kume, Tomonori
Tanaka, Nobuaki
Yoshifuji, Natsuko
Otsuki, Kyoichi
Suzuki, Masakazu
Kumagai, Tomo'omi
TI Modeling Seasonal Changes in the Temperature Lapse Rate in a Northern
Thailand Mountainous Area
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID INDO-CHINA PENINSULA; CRYPTOMERIA-JAPONICA PLANTATION; NOCTURNAL
DRAINAGE FLOW; DRY VALLEY SLOPES; SURFACE CONDUCTANCE; CANOPY
CONDUCTANCE; SLOPING FOREST; GROWING-SEASON; WATER-BALANCE; MONSOON
AB Temperature data in the mountain forest regions are often extrapolated from temperature data recorded at base stations at lower elevation. Such extrapolation is often based on elevation differences between target regions and base stations at low elevation assuming a constant temperature lapse rate throughout the year. However, this assumption might be problematic where slope circulation is active and decoupled from the regional circulation. To model the seasonal change in the lapse rate, the authors compared daily maximum (T-max) and minimum temperatures (T-min) observed at a mountain forest site (Kog-Ma; 1300-m altitude) with those observed at the bottom of the basin (Chiang-Mai; 314-m altitude) in northern Thailand, where slope circulation is active and decoupled from the regional circulation. The difference in T-max between Kog-Ma and Chiang-Mai (Delta T-max; Kog-Ma minus Chiang-Mai) was relatively unchanged throughout the year. However, the difference in T-min between Kog-Ma and Chiang-Mai (Delta T-min) changed seasonally. Thus, assuming a constant lapse rate throughout the year could cause large errors in extrapolating T-min data in mountainous areas in northern Thailand. The difference Delta T-min was related to nighttime net radiation (Rn), suggesting that nocturnal drainage flow affects the determination of Delta T-min. This relationship would be useful in formulating seasonal changes in the lapse rate for T-min. As Rn data are generally unavailable for meteorological stations, an index that relates to the lapse rate for T-min and is calculated from T-max and T-min data is proposed. This index might be useful for accurately estimating T-min values in mountainous regions in northern Thailand.
C1 [Komatsu, Hikaru; Yoshifuji, Natsuko; Otsuki, Kyoichi; Kumagai, Tomo'omi] Kyushu Univ, Kasuya Res Forest, Fukuoka 8112415, Japan.
[Hashimoto, Hirofumi] Calif State Univ Monterey Bay, Div Sci & Environm Policy, Seaside, CA USA.
[Hashimoto, Hirofumi] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kume, Tomonori] Natl Taiwan Univ, Sch Forestry & Resource Conservat, Taipei 10764, Taiwan.
[Tanaka, Nobuaki] Univ Tokyo, Grad Sch Agr & Life Sci, Univ Forests Aichi, Tokyo, Japan.
RP Komatsu, H (reprint author), Kyushu Univ, Kasuya Res Forest, 394 Tsubakuro, Fukuoka 8112415, Japan.
EM komatsu@forest.kyushu-u.ac.jp
RI Kumagai, Tomo'omi/A-4791-2011
FU Japanese Ministry of Education, Culture, Sports, Science and Technology
[20780119, 20248014]; Core Research for Evolution Science and Technology
of the Japan Science and Technology Agency
FX This research was supported by the Japanese Ministry of Education,
Culture, Sports, Science and Technology through a Grant-in-Aid for
Scientific Research (20780119 and 20248014) and by Core Research for
Evolution Science and Technology of the Japan Science and Technology
Agency. We express our great appreciation to the Thai Meteorological
Department and Prof. Jun Matsumoto (TokyoMetropolitan University, Japan)
for allowing us to use rainfall data recorded at Chiang-Mai. We also
thank Dr. Daisuke Komori (The University of Tokyo, Japan) and Dr.
Takehiko Satomura (Kyoto University, Japan) for describing the
instrumentation used at the Chiang-Mai station. We are grateful to Dr.
Yoshiyuki Miyazawa (Kyushu University, Japan) for fruitful discussion on
the photosynthesis of evergreen trees. We acknowledge three anonymous
reviewers for providing critical comments.
NR 66
TC 6
Z9 6
U1 1
U2 7
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD JUN
PY 2010
VL 49
IS 6
BP 1233
EP 1246
DI 10.1175/2010JAMC2297.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 634SC
UT WOS:000280604200011
ER
PT J
AU Priestley, KJ
Thomas, S
Smith, GL
AF Priestley, Kory J.
Thomas, Susan
Smith, G. Louis
TI Validation of Point Spread Functions of CERES Radiometers by the Use of
Lunar Observations
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID ENERGY SYSTEM CERES; CLOUDS
AB The Clouds and the Earth's Radiant Energy System (CERES) scanning radiometers have been operating to make raster scans of the moon on a quarterly basis to validate the point response function for the three channels of flight models 1-4 aboard the Terra and Aqua spacecraft. Instrument pointing accuracy was verified by this method to 0.28 for the total channel of FM-3. The point response functions were computed from the lunar observations and were found to be nominal with the exception of the FM-2 window channel, which was found to have a region of high sensitivity. This anomaly is attributed to a delamination of the detector flake from the heat sink in that region. The influence of this anomaly is accounted for by the in-flight calibration and has no adverse effect on the application of the data.
C1 [Priestley, Kory J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Thomas, Susan] Sci Syst Applicat Inc, Hampton, VA USA.
[Smith, G. Louis] Natl Inst Aerosp, Hampton, VA USA.
RP Priestley, KJ (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM g.louis.smith@nasa.gov
FU Earth Science Office of NASA; Sciences Directorate of the Langley
Research Center; National Institute for Aerospace
FX The authors gratefully acknowledge the support of the CERES Program by
the Earth Science Office of NASA and the Sciences Directorate of the
Langley Research Center for contract support of Science Systems
Applications, Inc. and National Institute for Aerospace.
NR 10
TC 10
Z9 10
U1 0
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD JUN
PY 2010
VL 27
IS 6
BP 1005
EP 1011
DI 10.1175/2010JTECHA1322.1
PG 7
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 615AR
UT WOS:000279103600005
ER
PT J
AU Kuttippurath, J
Kleinbohl, A
Bremer, H
Kullmann, H
Notholt, J
Sinnhuber, BM
Feng, WH
Chipperfield, M
AF Kuttippurath, Jayanarayanan
Kleinboehl, Armin
Bremer, Holger
Kuellmann, Harry
Notholt, Justus
Sinnhuber, Bjoern-Martin
Feng, Wuhu
Chipperfield, Martyn
TI Aircraft measurements and model simulations of stratospheric ozone and
N2O: implications for chemistry and transport processes in the models
SO JOURNAL OF ATMOSPHERIC CHEMISTRY
LA English
DT Article
DE Airborne measurements; Stratospheric ozone; Chemical transport model;
ASUR; CTMB; SLIMCAT; UCI; Parameterised chemistry
ID GENERAL-CIRCULATION MODEL; MIDLATITUDE STRATOSPHERE; TROPICAL
STRATOSPHERE; 3-DIMENSIONAL MODEL; MIDDLE ATMOSPHERE; SATELLITE DATA;
CLIMATOLOGY; VALIDATION; SPECTROMETER; TEMPERATURE
AB Airborne measurements of stratospheric ozone and N2O from the SCIAMACHY (Scanning Imaging Absorption Spectrometer) Validation and Utilization Experiment (SCIA-VALUE) are presented. The campaign was conducted in September 2002 and February-March 2003. The Airborne Submillimeter Radiometer (ASUR) observed stratospheric constituents like O-3 and N2O, among others, spanning a latitude from 5A degrees S to 80A degrees N during the survey. The tropical ozone source regions show high ozone volume mixing ratios (VMRs) of around 11 ppmv at 33 km altitude, and the altitude of the maximum VMR increases from the tropics to the Arctic. The N2O VMRs show the largest value of 325 ppbv in the lower stratosphere, indicating their tropospheric origin, and they decrease with increasing altitude and latitude due to photolysis. The sub-tropical and polar mixing barriers are well represented in the N2O measurements. The most striking seasonal difference found in the measurements is the large polar descent in February-March. The observed features are interpreted with the help of SLIMCAT and Bremen Chemical Transport Model (CTMB) simulations. The SLIMCAT simulations are in good agreement with the measured O-3 and N2O values, where the differences are within 1 ppmv for O-3 and 15 ppbv for N2O. However, the CTMB simulations underestimate the tropical middle stratospheric O-3 (1-1.5 ppmv) and the tropical lower stratospheric N2O (15-30 ppbv) measurements. A detailed analysis with various measurements and model simulations suggests that the biases in the CTMB simulations are related to its parameterised chemistry schemes.
C1 [Kuttippurath, Jayanarayanan] UPMC, LATMOS, CNRS, Paris, France.
[Kuttippurath, Jayanarayanan; Kleinboehl, Armin; Bremer, Holger; Kuellmann, Harry; Notholt, Justus; Sinnhuber, Bjoern-Martin] Univ Bremen, Inst Environm Phys, Bremen, Germany.
[Kleinboehl, Armin] NASA, JPL, CALTECH, Pasadena, CA USA.
[Bremer, Holger] Phys Tech Bundesanstalt, D-3300 Braunschweig, Germany.
[Sinnhuber, Bjoern-Martin] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany.
[Feng, Wuhu; Chipperfield, Martyn] Univ Leeds, Sch Environm, Leeds, W Yorkshire, England.
RP Kuttippurath, J (reprint author), UPMC, LATMOS, CNRS, 4 Pl Jussieu, Paris, France.
EM jayan@aero.jussieu.fr
RI Sinnhuber, Bjorn-Martin/A-7007-2013; Chipperfield, Martyn/H-6359-2013;
FENG, WUHU/B-8327-2008; Notholt, Justus/P-4520-2016
OI Sinnhuber, Bjorn-Martin/0000-0001-9608-7320; Chipperfield,
Martyn/0000-0002-6803-4149; FENG, WUHU/0000-0002-9907-9120; Notholt,
Justus/0000-0002-3324-885X
FU German contribution [FKZ 50EE 0022]; ESA [349]
FX The authors thank Dr. C. McLinden and Dr. S. Olsen for their discussion
about the parameterised chemistry schemes with them and for the UCI and
UCI-GISS model data. The HALOE v18 climatology was provided by Dr.
William Randel and is greatly appreciated. They also thank M. Milz, G.
Stiller and T. von Clarmann for the MIPAS IMK v3 data. JK thank Dr. Gang
Hong for Dr. Hong's help during the study period. The in-house Bremen
ozone climatology was acquired through
http://www.iup.physik.uni-bremen.de/gome/o3climatology. The authors
thank M. Weber and L.N. Lamsal for making available the climatology for
this study. The HALOE v19 data were downloaded from
http://haloe.gats-inc.com/home/index.php, the SHADOZ data from
http://croc.gsfc.nasa.gov/shadoz/, and the POAM-3 data from
http://wvms.nrl.navy.mil/POAM/poam.html. The authors thank the HALOE,
SHADOZ, and POAM scientific teams for their data. The project was funded
by the German contribution to the ENVISAT validation under the contract
FKZ 50EE 0022 and is a part of the ESA proposal A.O.ID 349.
NR 61
TC 2
Z9 2
U1 1
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-7764
EI 1573-0662
J9 J ATMOS CHEM
JI J. Atmos. Chem.
PD JUN
PY 2010
VL 66
IS 1-2
BP 41
EP 64
DI 10.1007/s10874-011-9191-4
PG 24
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 806ES
UT WOS:000293789700004
ER
PT J
AU Yu, JY
Kao, HY
Lee, T
AF Yu, Jin-Yi
Kao, Hsun-Ying
Lee, Tong
TI Subtropics-Related Interannual Sea Surface Temperature Variability in
the Central Equatorial Pacific
SO JOURNAL OF CLIMATE
LA English
DT Article
ID TROPOSPHERIC BIENNIAL OSCILLATION; EL-NINO; SOUTHERN-OSCILLATION;
MONSOON RAINFALL; OCEAN; ENSO; NONLINEARITY; CIRCULATIONS; ANOMALIES;
MODEL
AB Interannual sea surface temperature (SST) variability in the central equatorial Pacific consists of a component related to eastern Pacific SST variations (called Type-1 SST variability) and a component not related to them (called Type-2 SST variability). Lead-lagged regression and ocean surface-layer temperature balance analyses were performed to contrast their control mechanisms. Type-1 variability is part of the canonical, which is characterized by SST anomalies extending from the South American coast to the central Pacific, is coupled with the Southern Oscillation, and is associated with basinwide subsurface ocean variations. This type of variability is dominated by a major 4-5-yr periodicity and a minor biennial (2-2.5 yr) periodicity. In contrast, Type-2 variability is dominated by a biennial periodicity, is associated with local air-sea interactions, and lacks a basinwide anomaly structure. In addition, Type-2 SST variability exhibits a strong connection to the subtropics of both hemispheres, particularly the Northern Hemisphere. Type-2 SST anomalies appear first in the northeastern subtropical Pacific and later spread toward the central equatorial Pacific, being generated in both regions by anomalous surface heat flux forcing associated with wind anomalies. The SST anomalies undergo rapid intensification in the central equatorial Pacific through ocean advection processes, and eventually decay as a result of surface heat flux damping and zonal advection. The southward spreading of trade wind anomalies within the northeastern subtropics-to-central tropics pathway of Type-2 variability is associated with intensity variations of the subtropical high. Type-2 variability is found to become stronger after 1990, associated with a concurrent increase in the subtropical variability. It is concluded that Type-2 interannual variability represents a subtropical-excited phenomenon that is different from the conventional ENSO Type-1 variability.
C1 [Yu, Jin-Yi; Kao, Hsun-Ying] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Kao, HY (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM jyyu@uci.edu
RI Yu, Jin-Yi/G-3413-2011
OI Yu, Jin-Yi/0000-0001-6156-7623
FU NSF [ATM-0925396]; NASA [NNX06AF49H]; JPL [1290687]
FX We thank two anonymous reviewers and Dr. Shang-Ping Xie for their
constructive and helpful comments. This research was support by NSF
Grant ATM-0925396, NASA Grant NNX06AF49H, and JPL Subcontract 1290687.
The GECCO data was downloaded from http://www.ecco-group.org. Data
analyses were performed at University of California, Irvine's Earth
System Modeling Facility.
NR 36
TC 86
Z9 92
U1 5
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 JUN
PY 2010
VL 23
IS 11
BP 2869
EP 2884
DI 10.1175/2010JCLI3171.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 611AR
UT WOS:000278783300004
ER
PT J
AU Twigg, ME
Picard, YN
Caldwell, JD
Eddy, CR
Mastro, MA
Holm, RT
Neudeck, PG
Trunek, AJ
Powell, JA
AF Twigg, M. E.
Picard, Y. N.
Caldwell, J. D.
Eddy, C. R., Jr.
Mastro, M. A.
Holm, R. T.
Neudeck, P. G.
Trunek, A. J.
Powell, J. A.
TI Diffraction Contrast of Threading Dislocations in GaN and 4H-SiC
Epitaxial Layers Using Electron Channeling Contrast Imaging
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article; Proceedings Paper
CT 13th International Conference on Defects - Recognition, Imaging and
Physics in Semiconductors (DRIP XIII)
CY SEP 13-17, 2009
CL Oglebay, WV
SP Minerals, Met & Mat Soc, FEI, Semilab, Quantum Focus, Off Naval Res, Air Force Off Sci Res, Army Res Off
DE Dislocations; gallium nitride; silicon carbide; scanning electron
microscopy; electron channeling; electron diffraction
ID SURFACE
AB Forescattered electron channeling contrast imaging (ECCI) offers the potential for imaging and analyzing extended defects in a scanning electron microscope (SEM). Indeed, it is shown that ECCI is able to determine the Burgers vector of threading dislocations with the aid of carefully determined experimental parameters and accompanying image simulations. Simulations are compared with ECC images from samples with features that are relatively easily studied and modeled: those based on specially engineered 4H-SiC mesa substrates. These mesas serve as substrates for both homoepitaxial 4H-SiC layers and heteroepitaxial GaN layers in which images of threading dislocations (TDs) have been recorded using ECCI and found to strongly resemble diffraction contrast simulations of TD intensity profiles.
C1 [Twigg, M. E.; Picard, Y. N.; Caldwell, J. D.; Eddy, C. R., Jr.; Mastro, M. A.; Holm, R. T.] USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA.
[Picard, Y. N.] Carnegie Mellon Univ, Dept Mat Sci & Engn, Pittsburgh, PA 15213 USA.
[Neudeck, P. G.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Trunek, A. J.] OAI, Cleveland, OH 44135 USA.
[Powell, J. A.] Sest Inc, Cleveland, OH 44135 USA.
RP Twigg, ME (reprint author), USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA.
EM twigg@estd.nrl.navy.mil
RI Caldwell, Joshua/B-3253-2008;
OI Caldwell, Joshua/0000-0003-0374-2168; Picard, Yoosuf/0000-0002-2853-5213
NR 19
TC 6
Z9 6
U1 1
U2 6
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD JUN
PY 2010
VL 39
IS 6
BP 743
EP 746
DI 10.1007/s11664-010-1143-2
PG 4
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA 596UW
UT WOS:000277712000025
ER
PT J
AU Holdeman, JD
Clisset, JR
Moder, JP
AF Holdeman, J. D.
Clisset, J. R.
Moder, J. P.
TI Spreadsheet Calculations for Jets in Crossflow From Single and Opposed
Rows With Alternating Hole Sizes
SO JOURNAL OF ENGINEERING FOR GAS TURBINES AND POWER-TRANSACTIONS OF THE
ASME
LA English
DT Article
DE flow; jets
ID MULTIPLE JETS
AB The primary purpose of this study was to show the expected results for cases of single and opposed rows of jets from alternating large and small round holes. Previous publications demonstrated that the NASA empirical model gave results that were an excellent representation of mean experimental scalar results and that the model could confidently be used to investigate configurations for which results have not been published in the open literature. Calculations for cases of opposed rows of jets that would overpenetrate slightly in an inline configuration showed that better mixing was attained when one row was shifted to make a staggered configuration so that a small hole was opposite from a larger one. However, the result was no better than for an optimum inline configuration with all the holes of the same size. Staggering the rows does not make much difference in an optimum inline configuration. For all cases investigated, the dimensionless variance of the mixture fraction decreased significantly with increasing downstream distance, but, at a given downstream location, the variation between cases was small.
C1 [Moder, J. P.] NASA, Glenn Res Ctr, Prop Syst Div, Combust Branch, Cleveland, OH 44135 USA.
[Clisset, J. R.] Univ Florida, Gainesville, FL 32611 USA.
EM jjdholdeman@aol.com
FU NASA Glenn Research Center; United Technologies Research Center;
Michigan State University; University of California-Irvine; Gas Turbine
Combustion
FX The authors would particularly like to thank Mr. Richard E. Walker
(Aerojet Liquid Rocket Co., retired) and Dr. Ram Srinivasan (then of
Garrett Turbine Engine Co.) for their contributions to the NASA JIC
empirical model, and to Professor William E. Lear of the University of
Florida for suggesting that the original computer code, written in
Applesoft (R) BASIC on a 64K Apple //e (R), could be rendered in an
Excel (R) spreadsheet and for directing the development of the
spreadsheet at UF. The authors also wish to acknowledge the
contributions to the spreadsheet made by Mr. Gilbert F. Canton (then at
UF) and Mr. Joel P. Scheuer (then a LERCIP participant at NASA Glenn)
and appreciate the support and encouragement from Mr. Timothy D. Smith,
Dr. Clarence T. Chang, and Dr. C. John Marek (retired) at the NASA Glenn
Research Center, Mr. David S. Liscinsky of the United Technologies
Research Center, Professor John F. Foss of Michigan State University,
Professor G. Scott Samuelsen of the University of California-Irvine, and
the late Professor Arthur H. Lefebvre, author of Gas Turbine Combustion.
NR 12
TC 2
Z9 3
U1 0
U2 2
PU ASME-AMER SOC MECHANICAL ENG
PI NEW YORK
PA THREE PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0742-4795
J9 J ENG GAS TURB POWER
JI J. Eng. Gas. Turbines Power-Trans. ASME
PD JUN
PY 2010
VL 132
IS 6
AR 064502
DI 10.1115/1.4000129
PG 7
WC Engineering, Mechanical
SC Engineering
GA 576WS
UT WOS:000276181300020
ER
PT J
AU Mazarico, E
Neumann, GA
Rowlands, DD
Smith, DE
AF Mazarico, Erwan
Neumann, G. A.
Rowlands, D. D.
Smith, D. E.
TI Geodetic constraints from multi-beam laser altimeter crossovers
SO JOURNAL OF GEODESY
LA English
DT Article
DE Laser altimeter; Crossover; Orbit determination; Moon; Multi-beam
ID MARS GLOBAL SURVEYOR; NEAR-SHOEMAKER; GRAVITY-FIELD; MOON
AB The round-trip travel time measurements made by spacecraft laser altimeters are primarily used to construct topographic maps of the target body. The accuracy of the calculated bounce point locations of the laser pulses depends on the quality of the spacecraft trajectory reconstruction. The trajectory constraints from Doppler and range radio tracking data can be supplemented by altimetric "crossovers", to greatly improve the reconstruction of the spacecraft trajectory. Crossovers have been used successfully in the past (e.g., Mars Orbiter Laser Altimeter on Mars Global Surveyor), but only with single-beam altimeters. The same algorithms can be used with a multi-beam laser altimeter, but we present a method using the unique cross-track topographic information present in the multi-beam data. Those crossovers are especially adapted to shallow (small angle) intersections, as the overlapping area is large, reducing the inherent ambiguities of single-beam data in that situation. We call those "swath crossovers". They prove particularly useful in the case of polar-orbiting spacecraft over slowly rotating bodies, because all the non-polar crossovers have small intersection angles. To demonstrate this method, we perform a simplified simulation based on the Lunar Reconnaissance Orbiter (LRO) and its five-beam Lunar Orbiter Laser Altimeter. We show that swath crossovers over one lunar month can independently, from geometry alone, recover the imposed orbital perturbations with great accuracy (5 m horizontal, < 1 m vertical, about one order of magnitude smaller than the imposed perturbations). We also present new types of constraints that can be derived from the swath crossovers, and designed to be used in a precision orbit determination setup. In future work, we will use such multi-beam altimetric constraints with data from LRO.
C1 [Mazarico, Erwan; Neumann, G. A.; Rowlands, D. D.; Smith, D. E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Mazarico, Erwan] Oak Ridge Associated Univ, NASA Postdoctral Program, NASA GSFC, Oak Ridge, TN 37831 USA.
[Smith, D. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Mazarico, E (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM erwan.m.mazarico@nasa.gov
RI Rowlands, David/D-2751-2012; Neumann, Gregory/I-5591-2013; Mazarico,
Erwan/N-6034-2014
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X
FU NASA; Lunar Reconnaissance Orbiter project
FX EM 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 thank the Lunar
Reconnaissance Orbiter project for their support of this work. We thank
three anonymous reviewers for comments which improved the manuscript.
NR 19
TC 10
Z9 12
U1 1
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
J9 J GEODESY
JI J. Geodesy
PD JUN
PY 2010
VL 84
IS 6
BP 343
EP 354
DI 10.1007/s00190-010-0379-1
PG 12
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 594PU
UT WOS:000277550500001
ER
PT J
AU Ferguson, IM
Dracup, JA
Duffy, PB
Pegion, P
Schubert, S
AF Ferguson, Ian M.
Dracup, John A.
Duffy, Philip B.
Pegion, Philip
Schubert, Siegfried
TI Influence of SST Forcing on Stochastic Characteristics of Simulated
Precipitation and Drought
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; MOISTURE-RAINFALL FEEDBACK; NINO-SOUTHERN
OSCILLATION; WESTERN UNITED-STATES; LONG-TERM DROUGHT; US GREAT-PLAINS;
SOIL-MOISTURE; SEASONAL PREDICTION; GCM SIMULATIONS; NORTH-AMERICA
AB Recent studies demonstrate that ocean-atmosphere forcing by persistent sea surface temperature (SST) anomalies is a primary driver of seasonal-to-interannual hydroclimatic variability, including drought events. Other studies, however, conclude that although SST anomalies influence the timing of drought events, their duration and magnitude over continental regions is largely governed by land-atmosphere feedbacks. Here the authors evaluate the direct influence of SST anomalies on the stochastic characteristics of precipitation and drought in two ensembles of AGCM simulations forced with observed (interannually varying) monthly SST and their climatological annual cycle, respectively. Results demonstrate that ocean-atmosphere forcing contributes to the magnitude and persistence of simulated seasonal precipitation anomalies throughout the tropics but over few mid- and high-latitude regions. Significant autocorrelation of simulated seasonal anomalies over oceans is directly forced by persistent SST anomalies; over land, SST anomalies are shown to enhance autocorrelation associated with land-atmosphere feedbacks. SST anomalies are shown to have no significant influence on simulated drought frequency, duration, or magnitude over most midlatitude land regions. Results suggest that severe and sustained drought events may occur in the absence of persistent SST forcing and support recent conclusions that ocean-atmosphere forcing primarily influences the timing of drought events, while duration and magnitude are governed by other mechanisms such as land-atmosphere feedbacks. Further analysis is needed to assess the potential model dependence of results and to quantify the relative contribution of land-atmosphere feedbacks to the long-term stochastic characteristics of precipitation and drought.
C1 [Ferguson, Ian M.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
[Dracup, John A.] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA.
[Duffy, Philip B.] Climate Cent Inc, Palo Alto, CA USA.
[Duffy, Philip B.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Pegion, Philip; Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Ferguson, IM (reprint author), Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
EM imfergus@mines.edu
RI Pegion, Philip/E-5247-2012
NR 70
TC 6
Z9 6
U1 0
U2 8
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 JUN
PY 2010
VL 11
IS 3
BP 754
EP 769
DI 10.1175/2009JHM1132.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 618PI
UT WOS:000279367700011
ER
PT J
AU Entekhabi, D
Reichle, RH
Koster, RD
Crow, WT
AF Entekhabi, Dara
Reichle, Rolf H.
Koster, Randal D.
Crow, Wade T.
TI Performance Metrics for Soil Moisture Retrievals and Application
Requirements
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID LAND-SURFACE MODELS; REMOTE-SENSING FOOTPRINTS; FORECAST VERIFICATION;
TEMPORAL STABILITY; VARIABILITY; VEGETATION; DYNAMICS; CLIMATE; SGP97
AB Quadratic performance metrics such as root-mean-square error (RMSE) and time series correlation are often used to assess the accuracy of geophysical retrievals (satellite measurements) with respect to true fields. These metrics are related; nevertheless, each has advantages and disadvantages. In this study the authors explore the relation between the RMSE and correlation metrics in the presence of biases in the mean as well as in the amplitude of fluctuations (standard deviation) between estimated and true fields. Such biases are common, for example, in satellite retrievals of soil moisture and impose constraints on achievable and meaningful RMSE targets. Last, an approach is introduced for converting a requirement in an application's product into a corresponding requirement for soil moisture accuracy. The approach can help with the formulation of soil moisture measurement requirements. It can also help determine the utility of a given retrieval product for applications.
C1 [Entekhabi, Dara] MIT, Ralph M Parsons Lab Environm Sci & Engn, Cambridge, MA 02139 USA.
[Reichle, Rolf H.; Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Crow, Wade T.] ARS, USDA, Hydrol & Remote Sensing Lab, Beltsville, MD USA.
RP Entekhabi, D (reprint author), MIT, Ralph M Parsons Lab Environm Sci & Engn, 48-216G, Cambridge, MA 02139 USA.
EM darae@mit.edu
RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012
OI Koster, Randal/0000-0001-6418-6383
FU NASA
FX This study by members of the SMAP Science Definition Team was supported
by NASA funding for the SMAP project.
NR 27
TC 101
Z9 101
U1 2
U2 15
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 JUN
PY 2010
VL 11
IS 3
BP 832
EP 840
DI 10.1175/2010JHM1223.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 618PI
UT WOS:000279367700017
ER
PT J
AU Barringer, H
Rydeheard, D
Havelund, K
AF Barringer, Howard
Rydeheard, David
Havelund, Klaus
TI Rule Systems for Run-time Monitoring: from EAGLE to RULER
SO JOURNAL OF LOGIC AND COMPUTATION
LA English
DT Article
DE Run-time verification; rule systems; temporal logic; grammars
ID RUNTIME VERIFICATION; NORMAL-FORM; GRAMMARS; RETURNS; THEOREM; CALLS
AB In Barringer et al. (2004. Vol. 2937, LNCS), EAGLE was introduced as a general purpose rule-based temporal logic for specifying run-time monitors. A novel interpretative trace-checking scheme via stepwise transformation of an EAGLE monitoring formula was defined and implemented. However, even though EAGLE presents an elegant formalism for the expression of complex trace properties, EAGLE'S interpretation scheme is complex and appears difficult to implement efficiently. In this article, we introduce RULER, a primitive conditional rule-based system, which has a simple and easily implemented algorithm for effective run-time checking, and into which one can compile a wide range of temporal logics and other specification formalisms used for run-time verification. As a formal demonstration, we provide a translation scheme for linear-time propositional temporal logic with a proof of translation correctness. We then introduce a parameterized version of RULER, in which rule names may have rule-expression or data parameters, which then coincides with the same expressivity as EAGLE with data arguments. RULER with just rule-expression parameters extend the expressiveness of RULER strictly beyond the class of context-free languages. For the language classes expressible in propositional RULER, the addition of rule-expression and data parameters enables more compact translations. Finally, we outline a few simple syntactic extensions of 'core' RULER that can lead to further conciseness of specification but still enabling easy and efficient implementation.
C1 [Barringer, Howard; Rydeheard, David] Univ Manchester, Sch Comp Sci, Manchester M13 9PL, Lancs, England.
[Havelund, Klaus] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Barringer, H (reprint author), Univ Manchester, Sch Comp Sci, Oxford Rd, Manchester M13 9PL, Lancs, England.
EM howard.barringer@manchester.ac.uk; david.rydeheard@manchester.ac.uk;
klaus.havelund@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The work of this author was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 17
TC 36
Z9 36
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0955-792X
J9 J LOGIC COMPUT
JI J. Logic Comput.
PD JUN
PY 2010
VL 20
IS 3
SI SI
BP 675
EP 706
DI 10.1093/logcom/exn076
PG 32
WC Computer Science, Theory & Methods; Logic
SC Computer Science; Science & Technology - Other Topics
GA 613TN
UT WOS:000279004000003
ER
PT J
AU Hodges, DH
Rajagopal, A
Ho, JC
Yu, WB
AF Hodges, Dewey H.
Rajagopal, Anurag
Ho, Jimmy C.
Yu, Wenbin
TI STRESS AND STRAIN RECOVERY FOR THE IN-PLANE DEFORMATION OF AN ISOTROPIC
TAPERED STRIP-BEAM
SO JOURNAL OF MECHANICS OF MATERIALS AND STRUCTURES
LA English
DT Article
DE beam theory; elasticity; asymptotic methods
ID SECTION
AB The variational-asymptotic method was recently applied to create a beam theory for a thin strip-beam with a width that varies linearly with respect to the axial coordinate. For any arbitrary section, ratios of the cross-sectional stiffness coefficients to their customary values for a uniform beam depend on the rate of taper. This is because for a tapered beam the outward-directed normal to a lateral surface is not perpendicular to the longitudinal axis. This changes the lateral-surface boundary conditions for the cross-sectional analysis, in turn producing different formulae for the cross-sectional elastic constants as well as for recovery of stress, strain and displacement over a cross-section. The beam theory is specialized for the linear case and solutions are compared with those from plane-stress elasticity for stress, strain and displacement. The comparison demonstrates that for beam theory to yield such excellent agreement with elasticity theory, one must not only use cross-sectional elastic constants that are corrected for taper but also the corrected recovery formulae, which are in turn based on cross-sectional in-and out-of-plane warping corrected for taper.
C1 [Hodges, Dewey H.; Rajagopal, Anurag] Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA.
[Ho, Jimmy C.] NASA, Ames Res Ctr, Sci & Technol Corp, Moffett Field, CA 94035 USA.
[Yu, Wenbin] Utah State Univ, Dept Mech & Aerosp Engn, Logan, UT 84322 USA.
RP Hodges, DH (reprint author), Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, 270 Ferst Dr, Atlanta, GA 30332 USA.
EM dhodges@gatech.edu; r_anurag87@gatech.edu; jimmy.c.ho@us.army.mil;
wenbin@engineering.usu.edu
RI Yu, Wenbin/B-1916-2009
NR 8
TC 7
Z9 7
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 JUN
PY 2010
VL 5
IS 6
BP 963
EP 975
DI 10.2140/jomms.2010.5.963
PG 13
WC Materials Science, Multidisciplinary; Mechanics
SC Materials Science; Mechanics
GA 703XB
UT WOS:000286013500006
ER
PT J
AU Lyulin, OM
Kassi, S
Sung, K
Brown, LR
Campargue, A
AF Lyulin, O. M.
Kassi, S.
Sung, K.
Brown, L. R.
Campargue, A.
TI Determination of the low energy values of (CH4)-C-13 transitions in the
2 nu(3) region near 1.66 mu m from absorption spectra at 296 and 81 K
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Methane; CH4; (CH4)-C-13; Absorption spectroscopy; HITRAN; GOSAT;
Empirical lower states
ID MOLECULAR LINE PARAMETERS; SPECTROSCOPIC DATABASE; METHANE TRANSITIONS;
LASER SPECTROSCOPY; INFRARED-SPECTRUM; GLOBAL ANALYSIS; CM(-1);
STRENGTHS; BAND; (CO)-C-12-O-16
AB The high resolution absorption spectra of (CH4)-C-13 were recorded at 81 K by differential absorption spectroscopy using a cryogenic cell and a series of distributed feed back (DFB) diode lasers and at room temperature by Fourier transform spectroscopy. The investigated spectral region corresponds to the high energy part of the (CH4)-C-13 tetradecad dominated by the 2 nu(3) overtone near 5988 cm(-1). Empirical line lists were constructed containing, respectively, 1629 (CH4)-C-13 transitions detected at 81 K (5852-6124 cm(-1)) and 3481 features (including 85 lines of (CH4)-C-12) measured at room temperature (5850-6150 cm(-1)); the smallest measured intensities are about 3 x 10(-26) and 4 x 10(-25) cm/molecule at 81 and 296 K, respectively. The lower state energy values were derived for 1196 (CH4)-C-13 transitions from the variation of the line intensities between 81 and 296 K. These transitions represent 99.2% and 84.6% of the total absorbance in the region, at 81 and 296 K. respectively. Over 400 additional weak features were measured at 81 K and could not be matched to lines observed at room temperature. The quality of the resulting empirical low energy values is demonstrated by the excellent agreement with the already-assigned transitions and the clear propensity of the empirical low values to be close to integers. The two line lists at 81 and at 296 K provided as Supplementary material will enable future theoretical analyses of the upper (CH4)-C-13 tetradecad. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Lyulin, O. M.; Kassi, S.; Campargue, A.] Univ Grenoble 1, Spectrometrie Phys Lab, CNRS, UMR 5588, F-38402 St Martin Dheres, France.
[Sung, K.; Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lyulin, O. M.] Russian Acad Sci, Lab Theoret Spect, Inst Atmospher Opt, Siberian Branch, Tomsk 634055, Russia.
RP Campargue, A (reprint author), Univ Grenoble 1, Spectrometrie Phys Lab, CNRS, UMR 5588, BP 87, F-38402 St Martin Dheres, France.
EM Alain.Campargue@ujf-grenoble.fr
RI Sung, Keeyoon/I-6533-2015
FU ANR [BLAN08-2_321467]; RFBR [RFBR 09-05-92508-NKa]; CRDF
[RUG1-2954-TO-09]; Groupement de Recherche International SAMIA (France);
RFBR (Russia) [N 09-05-93105]; CAS (China)
FX O.M.L. (IAO, Tomsk) is grateful to the French Embassy in Moscow for a
two months visiting support at Grenoble University. This work is part of
the ANR project "CH4@Titan" (Ref: BLAN08-2_321467). The supports by RFBR
(Grant RFBR 09-05-92508-NKa), CRDF (Grant RUG1-2954-TO-09) and by the
Groupement de Recherche International SAMIA between CNRS (France), RFBR
(N 09-05-93105, Russia) and CAS (China) is acknowledged. Part of the
research described in this paper was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 37
TC 20
Z9 23
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 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD JUN
PY 2010
VL 261
IS 2
BP 91
EP 100
DI 10.1016/j.jms.2010.03.008
PG 10
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 610DM
UT WOS:000278710900004
ER
PT J
AU Nikolaev, P
Holmes, W
Sosa, E
Boul, P
Arepalli, S
Yowell, L
AF Nikolaev, Pavel
Holmes, William
Sosa, Edward
Boul, Peter
Arepalli, Sivaram
Yowell, Leonard
TI Effect of Vaporization Temperature on the Diameter and Chiral Angle
Distributions of Single-Walled Carbon Nanotubes
SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY
LA English
DT Article
DE Carbon; Nanotubes; Laser Ablation; Synthesis; Chiral Angle; Diameter
Mechanism
ID LASER-ABLATION PROCESS; CATALYTIC GROWTH; SEPARATION; DYNAMICS
AB Pulsed laser vaporization synthesis of single-wall carbon nanotubes on Co/Ni and Rh/Pd catalysts was explored with respect to variations in the production temperature. The nanotube type populations were determined via photoluminescence, UV-Vis-NIR absorption and Raman spectroscopy. It was found that lowered production temperature leads to smaller nanotube diameters and exceptionally narrow (n, m) type distributions, with marked preference towards large chiral angles for both catalysts. Interestingly, larger nanotube diameters tend to be associated with larger chiral angles. These results demonstrate that PLV production technique can provide at least partial control over the nanotube (n, m) populations. In addition, these results have implications for the understanding the nanotube nucleation mechanism in the laser oven. SWCNT synthesized at lower temperatures appear quite attractive as a starting material for nanotube type separation experiments.
C1 [Nikolaev, Pavel; Holmes, William; Sosa, Edward; Boul, Peter; Arepalli, Sivaram] NASA, Lyndon B Johnson Space Ctr, ERC Inc, Houston, TX 77258 USA.
RP Nikolaev, P (reprint author), Sungkyunkwan Univ, Dept Energy Sci, 300 Cheoncheon Dong, Suwon 440746, South Korea.
FU NASA [NNJ05HI05C]; State of Texas [SAA-AT-07-021, RAN 0798, UTA07-099]
FX Authors would like to acknowledge financial support from NASA under
contract #NNJ05HI05C and from State of Texas, Space Act Agreement
#SAA-AT-07-021 (RAN 0798) (UTA07-099). Authors thank R. Bruce Weisman of
Rice University for access to the Nanospectralyzer for photoluminescence
measurements.
NR 47
TC 9
Z9 9
U1 2
U2 15
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 JUN
PY 2010
VL 10
IS 6
SI SI
BP 3780
EP 3789
DI 10.1166/jnn.2010.2008
PG 10
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 569UC
UT WOS:000275626500006
PM 20355368
ER
PT J
AU Oye, MM
Yim, S
Fu, A
Schwanfelder, K
Meyyappan, M
Nguyen, CV
AF Oye, Michael M.
Yim, Setha
Fu, Alan
Schwanfelder, Kevin
Meyyappan, M.
Nguyen, Cattien V.
TI Surface Smoothness Effect for the Direct Growth of Carbon Nanotubes on
Bulk FeCrAl Metal Substrates
SO JOURNAL OF NANOSCIENCE AND NANOTECHNOLOGY
LA English
DT Article
DE Carbon Nanotube; FeCrAl; Bulk Metal Catalyst Substrate; Growth Morpholog
ID CHEMICAL-VAPOR-DEPOSITION; MECHANISMS; FILM
AB We investigate effects of surface smoothness and surface chemistry on the nature of multi-walled CNTs (MWCNTs) grown directly on FeCrAl substrates. A single sample was grown that contained a gradation in surface morphologies ranging from 2.9 nm to 30.2 nm RMS. The MWCNTs were grown using ethylene and H(2) gases. Characterization was done using atomic force microscopy (AFM), scanning electron microscopy (SEM), and Auger elemental surface analysis. In smooth regions, MWCNTs demonstrated high-density vertical aligned growths; however, patches of similar to 10-20 mu m where poor MWCNT growth occurred. In contrast, rough regions of the surface exhibited a continuous blanket layer of MWCNTs, albeit growth was spaghetti-like throughout this layer. The variation in nature of MWCNT growths was directly dependent on the surface roughness, which can affect surface growth chemistry of MWCNTs. Auger elemental analysis determined carbon was observed everywhere on the surface, but carbon was strongest over the smooth regions of high density growth; while relatively less carbon was detected over the patches with poor MWCNT growth, as well as over the blanket layer of the rough region. Oxygen was also measured, which was detected both within the patches of poor MWCNT growth in the smooth regions and over the blanket layer of the rough region. However, measurements of Cr and Al were exhibiting mixed trends: Cr was detected more strongly than Al over the rough region; whereas the opposite was observed in the patches of poor MWCNT growth in the smooth region. The surface smoothness affects the surface chemistry involving the nature of MWCNT growth and may also affect the surface chemistry involving the metal substrate itself; therefore, comparisons on the nature of MWCNT growths must also take careful consideration of the surface smoothness.
C1 [Oye, Michael M.; Yim, Setha; Fu, Alan; Schwanfelder, Kevin; Meyyappan, M.; Nguyen, Cattien V.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Nguyen, CV (reprint author), ELORET Corp, Sunnyvale, CA USA.
FU NASA
FX Work by Michael M. Oye, Setha Yim, Alan Fu, Kevin Schwanfelder, and
Cattien V. Nguyen was supported by a NASA contract to FLORET
Corporation. Michael M. Oye, Setha Yim, Kevin Schwanfelder, and Cattien
V. Nguyen are employed by FLORET Corporation (465 S. Mathilda Ave.;
Sunnyvale, CA 94086 USA). Alan Fu is a high school student intern from
Palo Alto High School (50 Embarcaderc, Rd.; Palo Alto, CA 94301 USA).
NR 18
TC 7
Z9 7
U1 1
U2 8
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 JUN
PY 2010
VL 10
IS 6
SI SI
BP 4082
EP 4088
DI 10.1166/jnn.2010.1991
PG 7
WC Chemistry, Multidisciplinary; Nanoscience & Nanotechnology; Materials
Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 569UC
UT WOS:000275626500057
PM 20355419
ER
PT J
AU Smith, MAH
Benner, DC
Predoi-Cross, A
Devi, VM
AF Smith, M. A. H.
Benner, D. Chris
Predoi-Cross, A.
Devi, V. Malathy
TI Multispectrum analysis of (CH4)-C-12 in the nu(4) spectral region: II.
Self-broadened half widths, pressure-induced shifts, temperature
dependences and line mixing
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Methane; Line broadening; Widths; Pressure-induced shifts; Off-diagonal
relaxation matrix elements; Line mixing; Temperature dependence
ID MOLECULAR SPECTROSCOPIC DATABASE; DIODE-LASER SPECTROSCOPY; BAND
Q-BRANCH; METHANE LINES; COEFFICIENTS WIDTHS; 4635 CM(-1); V(2) BAND;
ABSORPTION; CH4; (HCN)-C-12-N-14
AB Accurate values for line positions, absolute line intensities, self-broadened half width and self-pressure-induced shift coefficients have been measured for over 400 allowed and forbidden transitions in the nu 4 band of methane ((CH4)-C-12). Temperature dependences of half width and pressure-induced shift coefficients were also determined for many of these transitions. The spectra used in this study were recorded at temperatures between 210 and 314K using the National Solar Observatory's 1 m Fourier transform spectrometer at the McMath-Pierce solar telescope. The complete data set included 60 high-resolution (0.006-0.01 cm(-1)) absorption spectra of pure methane and methane mixed with dry air. The analysis was performed using a multispectrum nonlinear least squares curve fitting technique where a number of spectra (20 or more) were fit simultaneously in spectral intervals 5-15 cm(-1) wide. In addition to the line broadening and shift parameters, line mixing coefficients (using the off-diagonal relaxation matrix element formalism) were determined for more than 50 A-, E-, and F-species transition pairs in J manifolds of the P- and R-branches. The measured self-broadened half width and self-shift coefficients, their temperature dependences and the line mixing parameters are compared to self-broadening results available in the literature and to air-broadened parameters determined for these transitions from the same set of spectra. Published by Elsevier Ltd.
C1 [Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Williamsburg, VA 23187 USA.
[Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
RP Smith, MAH (reprint author), NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
EM Mary.Ann.H.Smith@NASA.gov
FU National Aeronautics and Space Administration; National Sciences and
Engineering Research Council of Canada (NSERC)
FX The authors thank Claude Plymate and Mike Dulick of the National Solar
Observatory for their assistance with the FTS laboratory measurements at
Kitt Peak. Research at the College of William and Mary is supported
under contracts and cooperative agreements with the National Aeronautics
and Space Administration. A. Predoi-Cross acknowledges the support
received from the National Sciences and Engineering Research Council of
Canada (NSERC). The authors thank NASA's Upper Atmospheres Research
Program for its support of the McMath-Pierce FTS laboratory facility. We
also thank Larry Rothman for his wise counsel and friendship over the
years of this study and many more.
NR 32
TC 16
Z9 16
U1 1
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUN
PY 2010
VL 111
IS 9
SI SI
BP 1152
EP 1166
DI 10.1016/j.jqsrt.2010.01.017
PG 15
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800010
ER
PT J
AU Drouin, BJ
Yu, SS
Miller, CE
Muller, HSP
Lewen, F
Bruenken, S
Habara, H
AF Drouin, Brian J.
Yu, Shanshan
Miller, Charles E.
Mueller, Holger S. P.
Lewen, Frank
Bruenken, Sandra
Habara, Hideta
TI Terahertz spectroscopy of oxygen, O-2, in its (3)Z(g)(-) and (1)Delta
electronic states THZ Spectroscopy of O-2
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Oxygen; Rotational spectroscopy; Terahertz spectroscopy; Atmospheric
species; O-16/O-18 ratio
ID SUBMILLIMETER-WAVE SPECTRUM; MICROWAVE-ABSORPTION LINES; BROAD-BAND
SPECTROSCOPY; GROUND-STATE; ATMOSPHERIC OXYGEN; ROTATIONAL TRANSITIONS;
MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; FINE-STRUCTURE; FREQUENCIES
AB High precision rotational spectra of isotopic oxygen O-2 (with O-16 or O-18) in its (3)Sigma(-)(g) electronic ground state have been measured in selected frequency regions between 0.4 and 2.0THz. The main isotopic species, O-16(2), was also investigated in its first excited electronic state (1)Delta. The new data, analyzed together with previous measurements, yielded improved spectroscopic parameters. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Drouin, Brian J.; Yu, Shanshan; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mueller, Holger S. P.; Lewen, Frank; Bruenken, Sandra; Habara, Hideta] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Brian.J.Drouin@jpl.nasa.gov; hspm@ph1.uni-koeln.de
RI Brunken, Sandra/B-1880-2010; Yu, Shanshan/D-8733-2016
OI Brunken, Sandra/0000-0001-7175-4828;
FU Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungs
Gemeinschaft (DFG) [SFB 494]; Land Nordrhein-Westfalen (NRW)
FX H.S.P.M. is grateful for recent support by the Bundesministerium fur
Bildung und Forschung (BMBF) administered by the Deutsches Zentrum fur
Luft- und Raumfahrt (DLR). This paper presents research carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. A large
portion of the work in Cologne was supported by the Deutsche Forschungs
Gemeinschaft (DFG) in the framework of the collaborative research grant
SFB 494. Additional support by the Land Nordrhein-Westfalen (NRW) is
also acknowledged.
NR 40
TC 18
Z9 18
U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUN
PY 2010
VL 111
IS 9
SI SI
BP 1167
EP 1173
DI 10.1016/j.jqsrt.2009.12.006
PG 7
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800011
ER
PT J
AU Gordon, IE
Kassi, S
Campargue, A
Toon, GC
AF Gordon, Iouli E.
Kassi, Samir
Campargue, Alain
Toon, Geoffrey C.
TI First identification of the a(1) Delta(g)-X-3 Sigma(-)(g) electric
quadrupole transitions of oxygen in solar and laboratory spectra
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Electric quadrupole; Singlet delta; Oxygen; Solar spectrum; Cavity ring
down spectroscopy
ID CAVITY RINGDOWN SPECTROSCOPY; LINE PARAMETERS COMPILATION; 1.5 MU-M;
ATMOSPHERIC OXYGEN; MOLECULAR-OXYGEN; BAND; INTENSITIES; EINSTEIN;
COEFFICIENTS; ISOTOPOMERS
AB Electric quadrupole transitions in the a(1)Delta(g)-X-3 Sigma(-)(g) band of O-16(2) near 1.27 mu m are reported for the first time. They were first detected in atmospheric solar spectra acquired with a ground-based Fourier transform spectrometer (FTS) in Park Falls, WI. Subsequently high-sensitivity ON cavity ring down spectroscopy (CW-CRDS) experiments were carried out at Grenoble University in the 7717-7917 cm(-1) region in order to provide quantitative intensity information for the electric quadrupole transitions. Measured intensities were used as input data for the calculation of the complete list of electric quadrupole transitions with Delta J= +/- 2, +/- 1 and 0. The calculation was carried out for the intermediate coupling case and assuming that these transitions are possible only through mixing of the Omega=0 component of the ground electronic state and b(1)Sigma(+)(g) state induced by spin-orbit coupling. The calculated line list agrees well with experimental measurements and was used to improve the residuals of the fitted solar atmospheric spectrum. Emission probability for the electric quadrupole band was determined to be (1.02 +/- 0.10) x 10(-6)s(-1). (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Kassi, Samir; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
EM igordon@cfa.harvard.edu
OI Gordon, Iouli/0000-0003-4763-2841
FU NASA; ANR; NASA EOS HITRAN
FX The authors are grateful to Rebecca Washenfelder and Jean-Francois
Blavier who set up the TCCON FTS at Park Falls, WI, and recorded the
atmospheric solar absorption spectra used here. We acknowledge Paul
Wennberg for the use of these data and the NASA Carbon Cycle program
which funds TCCON. We also thank Andrew Orr-Ewing for providing such a
good O2 magnetic dipole line list, that the missing
quadrupole lines became so prominent. We also thank Robert Field and
Charles Miller for fruitful discussions and Laurence Rothman and Robert
Gamache for providing input parameters and the program for calculation
of HITRAN line positions calculation. The HITRAN database managed for
over 35 years by Dr. Rothman is an essential tool in many fields. The
authors have all benefited from using it many times and are honored to
contribute to it or validate its data. Part of this work was performed
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with NASA and at Grenoble University under the ANR
project "IDEO". IEG is supported through NASA EOS HITRAN Grant.
NR 35
TC 22
Z9 22
U1 0
U2 11
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUN
PY 2010
VL 111
IS 9
SI SI
BP 1174
EP 1183
DI 10.1016/j.jqsrt.2010.01.008
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800012
ER
PT J
AU Toth, RA
Sung, K
Brown, LR
Crawford, TJ
AF Toth, Robert A.
Sung, Keeyoon
Brown, Linda R.
Crawford, Timothy J.
TI Line positions and strengths of 41 bands including 10 OCS isotopologues
in the 3850-4200 cm(-1) region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Carbonyl sulfide; OCS; Frequencies; Intensities; Strengths; Venus; Near
IR
ID FOURIER-TRANSFORM SPECTROSCOPY; HETERODYNE FREQUENCY MEASUREMENTS; LASER
PHOTOACOUSTIC-SPECTROSCOPY; CARBONYL SULFIDE; MU-M; INTENSITIES;
(OCS)-O-16-C-12-S-32; CO; SPECTRUM; DATABASE
AB The present analysis substantially improves the spectroscopic characterization of near infrared OCS in a window region (3850-4200 cm(-1)) important for atmospheric studies of Venus. Previous studies in this spectral region cataloged numerous OCS line positions, but accurate line intensities were measured for only three strong bands. In this paper, the corresponding line intensities are obtained for 41 OCS bands, including weak isotopic bands reported for the first time. The 2 nu(3) (0002-0000) band is analyzed for 10 OCS isotopologues (adding (OCS)-O-16-C-13-S-34, (OCS)-O-17-C-12-S-32, (OCS)-O-16-C-12-S-36, (OCS)-O-18-C-12-S-34, and (OCS)-O-16-C-13-S-33). In addition, observations of 0332-0330 of the main isotope, (OCS)-O-16-C-12-S-32, provides accurate vibration-rotation parameters for the upper state (and the lower state, 0330 of (OCS)-O-16-C-12-S-32). Finally, one unidentified band is seen at 3969.3 cm(-1); its lower state is clearly the ground state of (OCS)-O-16-C-12-S-32. S. The line strengths of these seven previously unanalyzed bands plus 34 other bands of the OCS isotopologues, (OCS)-O-16-C-12-S-32, (OCS)-O-16-C-12-S-34, (OCS)-O-16-C-13-S-32, (OCS)-O-16-C-12-S-33, and (OCS)-O-18-C-12-S-32, were least-squares fitted to determine strength parameters, S-v and Herman-Wallis coefficients. Finally, the intensities of 17 additional very weak bands were estimated to provide an extensive new database of OCS line parameters to support remote sensing of Venus. The integrated intensity in cm(-1)/(molecule cm(-2)) at 296 K is 8.1 x 10(-19) for the 3800-4200 cm(-1) region. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Toth, Robert A.; Sung, Keeyoon; Brown, Linda R.; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Toth, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MailStop 183-301, Pasadena, CA 91109 USA.
EM ratoth@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
NR 32
TC 6
Z9 6
U1 1
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUN
PY 2010
VL 111
IS 9
SI SI
BP 1193
EP 1208
DI 10.1016/j.jqsrt.2009.10.014
PG 16
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800014
ER
PT J
AU Devi, VM
Rinsland, CP
Benner, DC
Sams, RL
Blake, TA
AF Devi, V. Malathy
Rinsland, C. P.
Benner, D. Chris
Sams, R. L.
Blake, T. A.
TI Multispectrum analysis of the nu(9) band of (C2H6)-C-12: Positions,
intensities, self- and N-2-broadened half-width coefficients
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE 33.20.Ea
ID MOLECULAR SPECTROSCOPIC DATABASE; RESOLUTION INFRARED-SPECTRUM;
DIODE-LASER SPECTRA; NU-9 BAND; TEMPERATURE-DEPENDENCE; UPPER
TROPOSPHERE; ETHANE C2H6; MU-M; ATMOSPHERE; LINES
AB Line positions, intensities, Lorentz self- and N-2-broadened half-width coefficients have been measured for (P)Q(3), (P)Q(2), (P)Q(1), (R)Q(0), (R)Q(1), (R)Q(2), and (R)Q(3) sub-band transitions in the nu(9) fundamental band of (C2H6)-C-12. A multispectrum nonlinear least-squares fitting technique was used to fit up to 17 high-resolution (similar to 0.00156 cm(-1)), room temperature absorption spectra of pure (99.99% chemical purity) natural sample of ethane and lean mixtures of the high-purity ethane diluted with N-2. A Bruker IFS 120HR Fourier transform spectrometer located at the Pacific Northwest National Laboratory (PNNL), in Richland, Washington was used to record the data. A standard Voigt line shape was assumed to fit all the data since no line mixing or other non Voigt line shapes were required to fit any of the spectra used in the analysis. Short spectral intervals (similar to 2-2.5 cm(-1)) of all 17 spectra covering a specific (P)Q or (R)Q sub-band were fit simultaneously. For the first time in an ethane band, pressure-broadened half-width coefficients were determined for the torsional-split components. However, for better reliability of the retrieved coefficients for the weaker components (transitions with large intensity ratios of 4:1 or 3:1 for most K levels between the strong and weak components), constraints were used such that the half-width coefficients of both torsional-split components for a given J were identical for a specific broadening gas. No pressure-induced shift coefficients were necessary to fit the spectra to their noise level. The present study revealed for the first time the dependence of self- and N-2-broadened half-width coefficients upon the J, K quantum numbers of the transitions in ethane. A number of transitions belonging to the nu(9)+nu(4)-nu(4) and the nu(9)+2 nu(4)-2 nu(4) hot bands were also observed in the fitted regions and measurements were made when possible. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Rinsland, C. P.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
[Sams, R. L.; Blake, T. A.] Pacific NW Natl Lab, Richland, WA 99352 USA.
RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA.
EM malathy.d.venkataraman@larc.nasa.gov
FU Department of Energy's Office of Biological and Environmental research
located at Pacific Northwest National Laboratory (PNNL); United States
Department of Energy [DE-AC05-76RLO1830]; NASA; College of William and
Mary
FX The authors thank Dr. Jon T. Hougen from the National Institute of
Standards and Technology, Gaithersburg, MD for many useful discussions
on ethane molecule and selection rules, and also for reading the
manuscript and providing critical suggestions. The experimental data for
the present study were recorded at the W. R. Wiley Environmental
Molecular Sciences Laboratory, a National scientific user facility
sponsored by the Department of Energy's Office of Biological and
Environmental research located at Pacific Northwest National Laboratory
(PNNL). PNNL is operated for the United States Department of Energy by
the Battelle Memorial Institute under Contract DE-AC05-76RLO1830. NASA's
planetary atmospheres program supported the work performed at NASA
Langley Research Center and the College of William and Mary.
NR 38
TC 14
Z9 12
U1 0
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUN
PY 2010
VL 111
IS 9
SI SI
BP 1234
EP 1251
DI 10.1016/j.jqsrt.2009.10.017
PG 18
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800017
ER
PT J
AU Kuai, L
Natraj, V
Shia, RL
Miller, C
Yung, YL
AF Kuai, Le
Natraj, Vijay
Shia, Run-Lie
Miller, Charles
Yung, Yuk L.
TI Channel selection using information content analysis: A case study of
CO2 retrieval from near infrared measurements
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Retrieval; Channel selection; Information analysis; Carbon dioxide
ID SPECTROSCOPIC DATABASE; SOUNDERS; SPACE; MODEL; GOSAT
AB A major challenge in retrieving CO2 concentrations from thermal infrared remote sensing comes from the fact that measurements in the 4.3 and 15 mu m absorption bands (AIRS or TES) are sensitive to both temperature and CO2 variations. This complicates the selection of absorption channels with maximum CO2 concentration information content. In contrast, retrievals using near infrared (NIR) CO2 absorption bands are relatively insensitive to temperature and are most sensitive to changes of CO2 near the surface, where the sources and sinks are located. The Orbiting Carbon Observatory (OCO) was built to measure reflected sunlight in three NIR spectral regions (the 0.76 mu m O-2 A-band and two CO2 bands at 1.61 and 2.06 mu m). In an effort to significantly increase the speed of accurate CO2 retrieval algorithms for OCO, we performed an information content analysis to identify the 20 best channels from each CO2 spectral region to use in OCO retrievals. Retrievals using these 40 channels provide as much as 75% of the total CO2 information content compared to retrievals using all 1016 channels in each spectral region. The CO2 retrievals using our selected channels have a precision better than 0.1 ppm. This technique can be applied to the retrieval of other geophysical variables (e.g., temperature or CH4), or modified for other instruments, such as AIRS or TES. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Kuai, Le; Shia, Run-Lie; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Natraj, Vijay; Miller, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kuai, L (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM kl@gps.caltech.edu
FU Orbiting Carbon Observatory (OCO); NASA Earth System Science Pathfinder
(ESSP) mission
FX This research is supported by the Orbiting Carbon Observatory (OCO)
project, a NASA Earth System Science Pathfinder (ESSP) mission. The
authors would like to thank Denis O'Brien, Igor Polonsky and Chris
O'Dell from Colorado State University for providing us the orbit
simulator code and for helping with its development and maintenance, and
James McDuffie from the Jet Propulsion Laboratory (JPL) for providing
covariance information.
NR 33
TC 6
Z9 7
U1 2
U2 8
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 JUN
PY 2010
VL 111
IS 9
SI SI
BP 1296
EP 1304
DI 10.1016/j.jqsrt.2010.02.011
PG 9
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 593OY
UT WOS:000277469800023
ER
PT J
AU Hou, TH
Boston, KG
Baughman, JM
Walker, S
Johnston, WM
AF Hou, T. H.
Boston, K. G.
Baughman, J. M.
Walker, S.
Johnston, W. M.
TI Composite-to-composite Bonding using Scotch-Weld (TM) AF-555M Structural
Adhesive
SO JOURNAL OF REINFORCED PLASTICS AND COMPOSITES
LA English
DT Article
DE AF-555M adhesive; T800H/3900-2 composite; composite-to-composite
adhesive bonding; single-lap shear strength
AB Processing and properties of composite-to-composite bonding using Scotch-Weld (TM) AF-555M structural adhesive were investigated. Bonding surfaces of T800H/3900-2 composite were prepared by co-curing the dry and wet peel-plies. Surface topologies of the peel-plies and the co-cured composite surfaces were examined by microscopy, contour mapping using a coordinate measuring machine equipped with a ruby sphere probe, and contact angle goniometry. Curing of the adhesive was conducted in an autoclave or vacuum press at 177 degrees C (350 degrees F) for 2 h under 310 KPa (45 psi). Common bagging practices for composite fabrication in an autoclave were followed. It was found that a prolonged vacuum application (i.e., overnight) prior to the application of temperature and pressure was a critical element to produce porosity-free, high-quality bonds with this adhesive system. Following this procedure, a strong bond line was consistently produced, which routinely provided a single-lap shear strength more than 10% higher than the nominal value of the adhesive (i.e., 35.9 MPa or 5200 psi) when tested at room temperature. An adhesive failure mode at the interface was noted on the fractured surfaces of specimens with strong bonds whereas a premature cohesive failure mode was more evident for the specimens with weaker bonds, probably due to porosities in the bond lines. Photomicrographs showed that the weak single-lap shear strengths occurred on specimens with significant porosity in the bond line, apparently caused by entrapped air from insufficient vacuum application prior to curing. The results of this study are discussed herein.
C1 [Hou, T. H.; Boston, K. G.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Baughman, J. M.; Walker, S.; Johnston, W. M.] Lockheed Martin Engn & Serv Co, Hampton, VA 23666 USA.
RP Hou, TH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM tan-hung.hou-1@nasa.gov
NR 12
TC 1
Z9 1
U1 0
U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0731-6844
J9 J REINF PLAST COMP
JI J. Reinf. Plast. Compos.
PD JUN
PY 2010
VL 29
IS 11
BP 1702
EP 1711
DI 10.1177/0731684409341679
PG 10
WC Materials Science, Composites; Polymer Science
SC Materials Science; Polymer Science
GA 602DB
UT WOS:000278117600010
ER
PT J
AU Sehirlioglu, A
Sayir, A
Dynys, F
AF Sehirlioglu, Alp
Sayir, Ali
Dynys, Fred
TI Doping of BiScO3-PbTiO3 Ceramics for Enhanced Properties
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID HIGH-TEMPERATURE; ELECTRICAL-PROPERTIES; PIEZOELECTRIC SYSTEM;
DIELECTRIC ANOMALIES; (1-X)BISCO3-XPBTIO(3); MICROSTRUCTURE;
PIEZOCERAMICS
AB Compositional modification of ferroelectric BiScO3-PbTiO3 (BS-PT) ceramics was investigated by Zr-Sc center dot doping as a function of temperature and electric field. Zr doping decreased the Curie temperature; yet depoling temperature was higher as determined from the weak field measurements. Weight change measurements explain the difference in sintering behavior, emphasizing the effects of sacrificial powder on the defect structure. Possible mechanisms are discussed in collaboration with the crystal structure analysis. Pb'(Bi) replacement was shown as a possible charge balance mechanism. Pb'(Bi) is supported by the weight loss data, crystal structure analysis and the weak-field electrical and electromechanical measurements. However, high field measurements contradicted the postulated Pb'(Bi) mechanism. Unipolar and bipolar high field polarization, strain and dielectric constant measurements indicated that the donor doping creates A-site vacancies; a similar observation to Pb(Zr,Ti)O-3 (PZT)-based ceramics. At higher temperatures, the property dependence on the composition decreased suggesting that thermally assisted domain motion eliminated the dependence of the domain wall mobility on the extrinsic contributions (i.e., defect structure induced by doping). Effect of Zr-Sc center dot doping on electrical and electromechanical properties are reported and discussed as a function of temperature.
C1 [Sehirlioglu, Alp] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
[Sayir, Ali; Dynys, Fred] NASA, John Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sehirlioglu, A (reprint author), Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
EM alp.sehirlioglu@case.edu
FU Air Force Office of Scientific Research [FA 9550-06-1-0260]
FX This work was supported by Air Force Office of Scientific Research Grant
FA 9550-06-1-0260.
NR 33
TC 27
Z9 28
U1 1
U2 28
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-7820
EI 1551-2916
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD JUN
PY 2010
VL 93
IS 6
BP 1718
EP 1724
DI 10.1111/j.1551-2916.2010.03648.x
PG 7
WC Materials Science, Ceramics
SC Materials Science
GA 604WL
UT WOS:000278309100042
ER
PT J
AU Sippel, JA
Zhang, FQ
AF Sippel, Jason A.
Zhang, Fuqing
TI Factors Affecting the Predictability of Hurricane Humberto (2007)
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID ENSEMBLE KALMAN FILTER; TROPICAL CYCLONE INTENSITY; DOPPLER RADAR
OBSERVATIONS; SEA INTERACTION THEORY; MESOSCALE PREDICTABILITY; MOIST
CONVECTION; CYCLOGENESIS; DYNAMICS; PRECIPITATION; ASSIMILATION
AB This study uses ensemble Kalman filter analyses and short-range ensemble forecasts to study factors affecting the predictability of Hurricane Humberto, which made landfall along the Texas coast in 2007. Humberto is known for both its rapid intensification and extreme forecast uncertainty, which makes it an ideal case in which to examine the origins of tropical cyclone strength forecast error. Statistical correlation is used to determine why some ensemble members strengthen the incipient low into a hurricane and others do not. During the analysis period, it is found that variations in midlevel moisture, low-level convective instability, and strength of a front to the north of the cyclone likely lead to differences in net precipitation, which ultimately leads to storm strength spread. Stronger storms are favored when the atmosphere is more moist and unstable and when the front is weaker, possibly because some storms in the ensemble begin entraining cooler and drier postfrontal air during this period. Later during the free forecast, variable entrainment of postfrontal air becomes a leading cause of strength spread. Surface moisture differences are the primary contributor to intensity forecast differences, and convective instability differences play a secondary role. Eventually mature tropical cyclone dynamics and differences in landfall time result in very rapid growth of ensemble spread. These results are very similar to a previous study that investigated a 2004 Gulf of Mexico low with a different model and analysis technique, which gives confidence that they are relevant to tropical cyclone formation and intensification in general. Finally, the rapid increase in forecast uncertainty despite relatively modest differences in initial conditions highlights the need for ensembles and advanced data assimilation techniques.
C1 [Sippel, Jason A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Zhang, Fuqing] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
RP Sippel, JA (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD USA.
EM jason.sippel@nasa.gov
RI Zhang, Fuqing/E-6522-2010
OI Zhang, Fuqing/0000-0003-4860-9985
FU U.S. Office of Naval Research [N000140410471, N000140910526]; NSF
[ATM-084065]; Oak Ridge Associated Universities through a contract with
NASA
FX This research started as part of the first author's doctoral
dissertation at Texas A&M University and continued during the author's
tenure at NASA's Goddard Space Flight Center under the NASA Postdoctoral
Program. The authors have benefited from discussions with John
Nielsen-Gammon, Scott Braun, and Larry Carey. Thanks are also due to
Yonghui Weng for help on the ensemble simulation. Finally, the authors
appreciate comments that significantly improved this study from Journal
of the Atmospheric Sciences editor Shigeo Yoden, reviewer Ron
McTaggart-Cowan, and two anonymous reviewers. Research completed at
Texas A&M University was sponsored in by the U.S. Office of Naval
Research under Grants N000140410471 and N000140910526 and by NSF Grant
ATM-084065. The remaining work, completed under the NASA Postdoctoral
Program, was sponsored by Oak Ridge Associated Universities through a
contract with NASA.
NR 34
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U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD JUN
PY 2010
VL 67
IS 6
BP 1759
EP 1778
DI 10.1175/2010JAS3172.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 618PN
UT WOS:000279368200005
ER
PT J
AU Mishchenko, MI
AF Mishchenko, M. I.
TI The amplitude of the coherent backscattering intensity peak for discrete
random media: Effect of packing density
SO KINEMATICS AND PHYSICS OF CELESTIAL BODIES
LA English
DT Article
ID GALILEAN SATELLITES; POLARIZATION RATIOS; ENHANCEMENT FACTORS; LIGHT;
PARTICLES; JUPITER; DIFFUSE; LAYER
AB The amplitude of the coherent backscattering intensity peak is computed for a medium composed of densely packed, randomly positioned particles. The cyclical component of the Stokes reflection matrix at exactly the backscattering direction is expressed in terms of the ladder component, and the ladder component is rigorously computed by numerically solving the vector radiative transfer equation. The effect of packing density is accounted for by multiplying the single-scattering Mueller matrix by the static structure factor computed in the Percus-Yevick approximation. It is shown that increasing packing density can substantially reduce the amplitude of the copolarized coherent backscattering peak, especially for smaller particles, and can make it significantly lower than 2. The effect of packing density on the amplitude of the cross-polarized peak is significantly weaker.
C1 [Mishchenko, M. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Mishchenko, M. I.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
RI Mishchenko, Michael/D-4426-2012
FU NASA Radiation Sciences Program
FX The author is grateful to P.V. Litvinov, Yu.G. Shkuratov, V.P.
Tishkovets, and E.G. Yanovitskij for many fruitful discussions. Partial
funding for this research was provided by the NASA Radiation Sciences
Program managed by H. Maring.
NR 29
TC 0
Z9 0
U1 0
U2 2
PU ALLERTON PRESS INC
PI NEW YORK
PA 18 WEST 27TH ST, NEW YORK, NY 10001 USA
SN 0884-5913
J9 KINEMAT PHYS CELEST+
JI Kinemat. Phys. Celest. Bodies
PD JUN
PY 2010
VL 26
IS 3
BP 95
EP 103
DI 10.3103/S0884591310030013
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 619MQ
UT WOS:000279434700001
ER
PT J
AU Moczydlowska, M
Schopf, JW
Willman, S
AF Moczydlowska, Malgorzata
Schopf, J. William
Willman, Sebastian
TI Micro- and nano-scale ultrastructure of cell walls in Cryogenian
microfossils: revealing their biological affinity
SO LETHAIA
LA English
DT Article
DE Biological affinity; cell; wall; Cryogenian; microfossils;
ultrastructure.
ID HAEMATOCOCCUS-PLUVIALIS; NEOPROTEROZOIC ACRITARCHS; OUTER WALLS;
CHLOROPHYCEAE; AUSTRALIA; EDIACARAN; VOLVOX; ALGAE; VOLVOCALES;
CHLORELLA
AB Recently established protocols and methods in advanced microscopy and spectrometry applied to studies of ancient unicellular organic-walled microfossils of uncertain biological affinities (acritarchs) provide new evidence of the fine ultrastructure of cell walls and their biochemistry that support the interpretation of some such microfossils as photosynthesizing microalgae. The micro-scale and nanoscale ultrastructure of the cell walls of late Cryogenian sphaeromorphic acritarchs from the Chichkan Formation (Kazakhstan) revealed by the advanced techniques and studied originally by Kempe et al. (2005) is here further analysed and compared with that of modern microalgal analogues. On the basis of such comparison, we interpret the preserved cell wall ultrastructure to reflect original layering and lamination within sub-layers of the fossil wall, rather than being a result of taphonomic and diagenetic alteration. The outer thick layer represents the primary wall and the inner layer the secondary wall of the cell, whereas the laminated amorphous sub-layers, 10-20 nm in thickness and revealed by transmission electron and atomic force microscopy, are recognized as trilaminar sheath structure. Because two-layered cell walls, trilaminar sheaths and the position of the TLS within the fossil cell wall are characteristic of the mature developmental state in cyst morphogenesis in modern microalgae, we infer that the Chichkan sphaeromorphs are probably resting cells (aplanospores) of chlorophyceaen green microalgae from the order Volvocales. square Biological affinity, cell wall, Cryogenian, microfossils, ultrastructure.
C1 [Moczydlowska, Malgorzata; Willman, Sebastian] Uppsala Univ, Dept Earth Sci, S-75236 Uppsala, Sweden.
[Schopf, J. William] Univ Calif Los Angeles, Dept Earth & Space Sci, Ctr Study Evolut & Origin Life, Inst Geophys & Planetary Phys,Mol Biol Inst, Los Angeles, CA 90095 USA.
[Schopf, J. William] Univ Calif Los Angeles, NASA, Astrobiol Inst, Los Angeles, CA 90095 USA.
RP Moczydlowska, M (reprint author), Uppsala Univ, Dept Earth Sci, Villavagen 16, S-75236 Uppsala, Sweden.
EM malgo.vidal@pal.uu.se; schopf@ess.ucla.edu; sebastian.willman@geo.uu.se
FU Swedish Research Council (Vetenskapsradet) [621-2004-5316]; CSEOL
(UCLA/IGPP Center for the Study of Evolution and the Origin of Life);
NASA Astrobiology Institute; Elsevier
FX Research by M. Moczydlowska and S. Willman was supported through the
Swedish Research Council (Vetenskapsradet) grant No. 621-2004-5316 to M.
Moczydlowska. The study has been inspired during the discussions with
colleagues participating in the World Summit on Ancient Microscopic
Fossils, 27 July to 2 August 2008, University of California, Los
Angeles, organized by J. William Schopf and supported by CSEOL
(UCLA/IGPP Center for the Study of Evolution and the Origin of Life),
NASA Astrobiology Institute, and Elsevier.
NR 54
TC 13
Z9 15
U1 1
U2 19
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0024-1164
J9 LETHAIA
JI Lethaia
PD JUN
PY 2010
VL 43
IS 2
BP 129
EP 136
DI 10.1111/j.1502-3931.2009.00175.x
PG 8
WC Paleontology
SC Paleontology
GA 591TX
UT WOS:000277328700001
ER
PT J
AU Joy, KH
Crawford, IA
Russell, SS
Kearsley, AT
AF Joy, Katherine H.
Crawford, Ian A.
Russell, Sara S.
Kearsley, Anton T.
TI Lunar meteorite regolith breccias: An in situ study of impact melt
composition using LA-ICP-MS with implications for the composition of the
lunar crust
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MILLER RANGE 05035; AL GANI 400; PECORA ESCARPMENT-02007; BOMBARDMENT
HISTORY; IRON CONCENTRATION; CENTRAL-HIGHLANDS; ICEFIELD 02205; MARE
BASALTS; MOON; SURFACE
AB Dar al Gani (DaG) 400, Meteorite Hills (MET) 01210, Pecora Escarpment (PCA) 02007, and MacAlpine Hills (MAC) 88104/88105 are lunar regolith breccia meteorites that provide sampling of the lunar surface from regions of the Moon that were not visited by the US Apollo or Soviet Luna sample return missions. They contain a heterogeneous clast population from a range of typical lunar lithologies. DaG 400, PCA 02007, and MAC 88104/88105 are primarily feldspathic in nature, and MET 01210 is composed of mare basalt material mixed with a lesser amount of feldspathic material. Here we present a compositional study of the impact melt and impact melt breccia clast population (i.e., clasts that were generated in impact cratering melting processes) within these meteorites using in situ electron microprobe and LA-ICP-MS techniques. Results show that all of the meteorites are dominated by impact lithologies that are relatively ferroan (Mg#(< 70)), have high Sc/Sm ratios (typically > 10), and have low incompatible trace element (ITE) concentrations (i.e., typically < 3.2 ppm Sm, < 1.5 ppm Th). Feldspathic impact melt in DaG 400, PCA 02007, and MAC 88104/05 are similar in composition to that estimated composition for upper feldspathic lunar crust (Korotev et al. 2003). However, these melt types are more mafic (i.e., less Eu, less Sr, more Sc) than feldspathic impact melts returned by the Apollo 16 mission (e.g., the group 3 and 4 varieties). Mafic impact melt clasts are common in MET 01210 and less common in PCA 02007 and MAC 88104/05. We show that unlike the Apollo mafic impact melt groups (Jolliff 1998), these meteorite impact melts were not formed from melting large amounts of KREEP-rich (typically > 10 ppm Sm), High Magnesium Suite (typically > 70 Mg#) or High Alkali Suite (high ITEs, Sc/Sm ratios < 2) target rocks. Instead the meteorite mafic melts are more ferroan, KREEP-poor and Sc-rich, and represent mixing between feldspathic lithologies and low-Ti or very low-Ti (VLT) basalts. As PCA 02007 and MAC 88104/05 were likely sourced from the Outer-Feldspathic Highlands Terrane our findings suggest that these predominantly feldspathic regions commonly contain a VLT to low-Ti basalt contribution.
C1 [Joy, Katherine H.; Crawford, Ian A.] Joint UCL Birkbeck Res Sch Earth Sci, Ctr Planetary Sci, London WC1E 6BT, England.
[Joy, Katherine H.; Russell, Sara S.; Kearsley, Anton T.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England.
[Joy, Katherine H.] USRA, Ctr Lunar Sci & Explorat, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Joy, Katherine H.] NASA, Lunar Sci Inst, Washington, DC USA.
[Crawford, Ian A.] Birkbeck Coll, Dept Earth & Planetary Sci, London WC1E 7HX, England.
RP Joy, KH (reprint author), Joint UCL Birkbeck Res Sch Earth Sci, Ctr Planetary Sci, Gower St, London WC1E 6BT, England.
EM joy@lpi.usra.edu
RI Crawford, Ian/H-7510-2012;
OI Crawford, Ian/0000-0001-5661-7403; Joy, Katherine/0000-0003-4992-8750
FU Leverhulme Trust; STFC; LPI/NLSI
FX Many thanks to Guy Consolmango and the Vatican Observatory for loaning
the DaG 400 sample to the NHM and to MWG/NASA for the loan of Antarctic
samples. Many thanks also to Mr. John Spratt (NHM), Dr. Sarah James
(formally of the NHM), and Dr. Andy Beard (Birkbeck/UCL) for their
assistance with analytical procedures. Many thanks for thorough reviews
and helpful comments of Drs. Randy Korotev, James Day, Jeff Taylor,
Barbara Cohen, Christian Koeberl, and an anonymous reviewer. We would
like to acknowledge the resources made available through the Lunar
Meteorite List Website (Randy Korotev), the Lunar Meteorite Compendium
(Kevin Righter), the Lunar Sample Compendium (Chuck Meyer), and the
Virtual Moon Atlas. Thanks to the Leverhulme Trust, STFC, and LPI/NLSI
for financial support. This is LPI contribution number 1600.
NR 139
TC 25
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U1 2
U2 14
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUN
PY 2010
VL 45
IS 6
BP 917
EP 946
DI 10.1111/j.1945-5100.2010.01067.x
PG 30
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 656XJ
UT WOS:000282374100001
ER
PT J
AU Hung, CC
McNatt, J
AF Hung, Ching-Cheh
McNatt, Jeremiah
TI Synthesis and stability of iron nanoparticles for lunar environment
studies
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SIMULATION
AB Simulants of lunar dust are needed when researching the lunar environment. However, unlike the true lunar dust, today's simulants do not contain nanophase iron. Two different processes have been developed to fabricate nanophase iron to be used as part of a lunar dust simulant. (1) The first is to sequentially treat a mixture of ferric chloride, fluorinated carbon, and soda lime glass beads at about 300 degrees C in nitrogen, at room temperature in air, and then at 1050 degrees C in nitrogen. The product includes glass beads that are gray in color, can be attracted by a magnet, and contains alpha-iron nanoparticles (which seem to slowly lose their lattice structure in ambient air during a period of 12 months). This product may have some similarity to the lunar glassy agglutinate, which contains FeO. (2) The second is to heat a mixture of carbon black and a lunar simulant (a mixed metal oxide that includes iron oxide) at 1050 degrees C in nitrogen. This process simulates lunar dust reactions with the carbon in a micrometeorite at the time of impact. The product contains a chemically modified simulant that can be attracted by a magnet and has a surface layer whose iron concentration increased during the reaction. The iron was found to be alpha-iron and Fe(3)O(4) nanoparticles, which appear to grow after the fabrication process. This growth became undetectable after 6 months of ambient air storage, but may last for several years or longer.
C1 [Hung, Ching-Cheh; McNatt, Jeremiah] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Hung, CC (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 309-2, Cleveland, OH 44135 USA.
EM ching-cheh.hung-1@nasa.gov
FU NASA Glenn Research Center; NASA GRC
FX The authors would like to acknowedge J. Gaier, A. Hepp, and K. Street
for fruitful discussions regarding this work. We appreciate the efforts
of D. Hull for the TEM work, as well as the efforts of R. Rogers, R.
Mattingly, and the late R. Garlick for producing XRD data of iron
nanoparticles over a 14 yr period. We are thankful for the financial
support of the NASA Glenn Research Center's Independent Research and
Development (IR&D) program and NASA GRC In Situ Resource Utilization
Project (ISRU-Roxygen).
NR 12
TC 0
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U1 0
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUN
PY 2010
VL 45
IS 6
BP 965
EP 972
DI 10.1111/j.1945-5100.2010.01075.x
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 656XJ
UT WOS:000282374100003
ER
PT J
AU Chaban, GM
Pizzarello, S
AF Chaban, Galina M.
Pizzarello, Sandra
TI Ab initio calculations of 6-and 7-carbon meteoritic amino acids and
their diastereomers
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID MURCHISON METEORITE; DEUTERIUM ENRICHMENT; CHEMISTRY
AB To better explain the unusual distribution and relative abundances of several 6- and 7-carbon amino acids found in meteorites, their thermodynamic properties were studied using accurate ab initio techniques. In addition to optimized structures and relative energies, vibrational frequency and thermochemical analysis of different diastereomers were performed at temperatures relevant to conditions of synthesis of these amino acids in meteorites. The results of calculations were compared with the measured content of the amino acids in the Murchison meteorite. The distribution of several longer chain amino acids in meteorites seems to point to at least some thermodynamic control in their formation. For diastereomeric compounds, on the other hand, the comparison suggests that their synthetic conditions, or those of their precursors, were far from thermodynamic equilibrium.
C1 [Chaban, Galina M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pizzarello, Sandra] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
RP Chaban, GM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM galina.m.chaban@nasa.gov
FU NASA Astrobiology and Exobiology Program
FX We would like to thank NASA Science Mission Directorate for computer
time award on the NASA Advanced Supercomputing facility at the NASA Ames
Research Center. This work was supported in part (S. P.) by the NASA
Astrobiology and Exobiology Program.
NR 17
TC 2
Z9 2
U1 0
U2 4
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUN
PY 2010
VL 45
IS 6
BP 1053
EP 1060
DI 10.1111/j.1945-5100.2010.01083.x
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 656XJ
UT WOS:000282374100008
ER
PT J
AU Ghoshal, A
Prosser, WH
Kim, HS
Chattopadhyay, A
Copeland, B
AF Ghoshal, Anindya
Prosser, William H.
Kim, Heung Soo
Chattopadhyay, Aditi
Copeland, Ben
TI Development of embedded piezoelectric acoustic sensor array architecture
SO MICROELECTRONICS RELIABILITY
LA English
DT Article
ID COMPOSITE STRUCTURES; LAMB WAVES; PLATES; SCATTERING; DAMAGE; MODE
AB This paper examines development of novel piezoelectric acoustic sensors, which are capable of sensing high frequency acoustic emissions in a composite/metallic plate. The fabrication of the piezoelectric acoustic sensors, made from piezoceramic ribbons, is described in the paper. An attempt was made to build directionality into the sensing system itself. Continuous sensors placed at right angles on a plate are discussed as a new approach to measure and locate the source of the acoustic waves. Novel signal processing algorithms based on bio-inspired neural systems for spatial filtering of large numbers of embedded sensor arrays in laminated composite media are presented. It is expected that the present work would help in the development of microelectronic sensing aiding diagnostics and prognostics techniques for highly efficient health monitoring of integrated aerospace vehicles and structures. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Ghoshal, Anindya] United Technol Res Ctr, E Hartford, CT 06108 USA.
[Prosser, William H.] NASA, Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA.
[Kim, Heung Soo] Dongguk Univ Seoul, Dept Mech Robot & Energy Engn, Seoul 100715, South Korea.
[Chattopadhyay, Aditi] Arizona State Univ, Dept Mech & Aerosp Engn, Tempe, AZ 85287 USA.
[Copeland, Ben] NASA, Langley Res Ctr, Mat Branch, Hampton, VA 23681 USA.
RP Ghoshal, A (reprint author), United Technol Res Ctr, 411 Silver Lane,MS 129-73, E Hartford, CT 06108 USA.
EM anindo_ghoshal@yahoo.com
RI Kim, Heung Soo /F-6611-2011
OI Kim, Heung Soo /0000-0001-7057-5174
NR 25
TC 7
Z9 7
U1 2
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0026-2714
J9 MICROELECTRON RELIAB
JI Microelectron. Reliab.
PD JUN
PY 2010
VL 50
IS 6
BP 857
EP 863
DI 10.1016/j.microrel.2010.01.037
PG 7
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Physics, Applied
SC Engineering; Science & Technology - Other Topics; Physics
GA 609GQ
UT WOS:000278644400016
ER
PT J
AU Andrews, JC
Almeida, E
van der Meulen, MCH
Alwood, JS
Lee, C
Liu, YJ
Chen, J
Meirer, F
Feser, M
Gelb, J
Rudati, J
Tkachuk, A
Yun, WB
Pianetta, P
AF Andrews, Joy C.
Almeida, Eduardo
van der Meulen, Marjolein C. H.
Alwood, Joshua S.
Lee, Chialing
Liu, Yijin
Chen, Jie
Meirer, Florian
Feser, Michael
Gelb, Jeff
Rudati, Juana
Tkachuk, Andrei
Yun, Wenbing
Pianetta, Piero
TI Nanoscale X-Ray Microscopic Imaging of Mammalian Mineralized Tissue
SO MICROSCOPY AND MICROANALYSIS
LA English
DT Article
DE X-ray microscopy; imaging; bone ultrastructure; bone mineral density;
trabeculae; lacuna; osteocyte
ID ATOMIC-FORCE MICROSCOPY; LACUNAR-CANALICULAR SYSTEM; LASER-SCANNING
MICROSCOPY; COMPUTED-TOMOGRAPHY; BONE-STRUCTURE; IN-SITU; MICROCOMPUTED
TOMOGRAPHY; ELECTRON-MICROSCOPY; TRABECULAR BONE; CELLS
AB A novel hard transmission X-ray microscope (TXM) at the Stanford Synchrotron Radiation Light-source operating from 5 to 15 keV X-ray energy with 14 to 30 mu m(2) field of view has been used for high-resolution (30-40 nm) imaging and density quantification of mineralized tissue. TXM is uniquely suited for imaging of internal cellular structures and networks in mammalian mineralized tissues using relatively thick (50 mu m), untreated samples that preserve tissue micro-and nanostructure. To test this method we performed Zernike phase contrast and absorption contrast imaging of mouse cancellous bone prepared under different conditions of in vivo loading, fixation, and contrast agents. In addition, the three-dimensional structure was examined using tomography. Individual osteocytic lacunae were observed embedded within trabeculae in cancellous bone. Extensive canalicular networks were evident and included processes with diameters near the 30-40 nm instrument resolution that have not been reported previously. Trabecular density was quantified relative to rod-like crystalline apatite, and rod-like trabecular struts were found to have 51-54% of pure crystal density and plate-like areas had 44-53% of crystal density. The nanometer resolution of TXM enables future studies for visualization and quantification of ultrastructural changes in bone tissue resulting from osteoporosis, dental disease, and other pathologies.
C1 [Andrews, Joy C.; Pianetta, Piero] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA.
[Almeida, Eduardo] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[van der Meulen, Marjolein C. H.] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Alwood, Joshua S.] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
[Lee, Chialing] San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA.
[Liu, Yijin] Inst High Energy Phys, Beijing 100039, Peoples R China.
[Chen, Jie] Univ Sci & Technol China, Natl Synchrotron Radiat Lab, Hefei 230026, Peoples R China.
[Meirer, Florian] Vienna Univ Technol, Inst Atom & Subatom Phys, Vienna, Austria.
[Feser, Michael; Gelb, Jeff; Rudati, Juana; Tkachuk, Andrei; Yun, Wenbing] Xradia Inc, Concord, CA 94520 USA.
RP Andrews, JC (reprint author), SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA.
EM jandrews@slac.stanford.edu
RI van der Meulen, Marjolein/D-1549-2010; Liu, Yijin/O-2640-2013; Meirer,
Florian/H-7642-2016
OI van der Meulen, Marjolein/0000-0001-6637-9808; Liu,
Yijin/0000-0002-8417-2488; Meirer, Florian/0000-0001-5581-5790
FU National Institutes of Health (NIH)/National Institute of Biomedical
Imaging and Bioengineering [R01-EB004321]; NIH [R01-AG028664]; National
Aeronautics and Space Administration [RAD2004-0000-0110]; Department of
Energy, Office of Basic Energy Sciences
FX This work has been supported by the National Institutes of Health
(NIH)/National Institute of Biomedical Imaging and Bioengineering grant
number R01-EB004321. Mouse loading experiments were supported by NIH
grant number R01-AG028664 (to M. C. H. M.) and E.A. is supported by
National Aeronautics and Space Administration Grant number
RAD2004-0000-0110. SSRL is supported by the Department of Energy, Office
of Basic Energy Sciences.
NR 47
TC 53
Z9 53
U1 1
U2 39
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1431-9276
J9 MICROSC MICROANAL
JI Microsc. microanal.
PD JUN
PY 2010
VL 16
IS 3
BP 327
EP 336
DI 10.1017/S1431927610000231
PG 10
WC Materials Science, Multidisciplinary; Microscopy
SC Materials Science; Microscopy
GA 599HS
UT WOS:000277902600011
PM 20374681
ER
PT J
AU Hochhalter, JD
Littlewood, DJ
Christ, RJ
Veilleux, MG
Bozek, JE
Ingraffea, AR
Maniatty, AM
AF Hochhalter, J. D.
Littlewood, D. J.
Christ, R. J., Jr.
Veilleux, M. G.
Bozek, J. E.
Ingraffea, A. R.
Maniatty, A. M.
TI A geometric approach to modeling microstructurally small fatigue crack
formation: II. Physically based modeling of microstructure-dependent
slip localization and actuation of the crack nucleation mechanism in AA
7075-T651
SO MODELLING AND SIMULATION IN MATERIALS SCIENCE AND ENGINEERING
LA English
DT Article
ID STRUCTURALLY SMALL CRACKS; CRITICAL PLANE APPROACH; ALUMINUM-ALLOY;
CRYSTAL PLASTICITY; LIFE PREDICTION; CYCLE FATIGUE; GROWTH; INCLUSIONS;
INITIATION; DAMAGE
AB The objective of this paper is to develop further a framework for computationally modeling microstructurally small fatigue crack growth in AA 7075-T651 (Bozek et al 2008 Modelling Simul. Mater. Sci. 16 065007). The focus is on the nucleation event, when a crack extends from within a second-phase particle into a surrounding grain, since this has been observed to be an initiating mechanism for fatigue crack growth in this alloy. It is hypothesized that nucleation can be predicted by computing a non-local nucleation metric near the crack front. The hypothesis is tested by employing a combination of experimentation and finite element modeling in which various slip-based and energy-based nucleation metrics are tested for validity, where each metric is derived from a continuum crystal plasticity formulation. To investigate each metric, a non-local procedure is developed for the calculation of nucleation metrics in the neighborhood of a crack front. Initially, an idealized baseline model consisting of a single grain containing a semi-ellipsoidal surface particle is studied to investigate the dependence of each nucleation metric on lattice orientation, number of load cycles and non-local regularization method. This is followed by a comparison of experimental observations and computational results for microstructural models constructed by replicating the observed microstructural geometry near second-phase particles in fatigue specimens. It is found that orientation strongly influences the direction of slip localization and, as a result, influences the nucleation mechanism. Also, the baseline models, replication models and past experimental observation consistently suggest that a set of particular grain orientations is most likely to nucleate fatigue cracks. It is found that a continuum crystal plasticity model and a non-local nucleation metric can be used to predict the nucleation event in AA 7075-T651. However, nucleation metric threshold values that correspond to various nucleation governing mechanisms must be calibrated.
C1 [Hochhalter, J. D.; Veilleux, M. G.; Bozek, J. E.; Ingraffea, A. R.] Cornell Univ, Cornell Fracture Grp, Ithaca, NY 14853 USA.
[Littlewood, D. J.] Sandia Natl Labs, Albuquerque, NM 87185 USA.
[Christ, R. J., Jr.] Northrop Grumman Integrated Syst, Technol Dev, Bethpage, NY 11714 USA.
[Maniatty, A. M.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
RP Hochhalter, JD (reprint author), NASA, Langley Res Ctr, Durabil Damage Tolerance & Reliabil Branch, MS 188E, Hampton, VA 23681 USA.
EM Jacob.D.Hochhalter@nasa.gov
FU Defense Advanced Research Projects Agency [HR0011-04-C-0003]; NASA
[ARMD-NNX07AB69A]
FX This paper is dedicated to Dr John Papazian, who passed away before
seeing its publication. John assembled, and was inspirational leader of,
our research team. His keen insights, always timely suggestions and warm
collegiality will be missed. The authors would also like to thank
Professor Anthony Rollett for his involved discussions and guidance.
This work is partially sponsored by the Defense Advanced Research
Projects Agency under contract HR0011-04-C-0003. Dr Leo Christodoulou is
the DARPA Program Manager. This work is also partially funded by NASA
under contract ARMD-NNX07AB69A. Dr Ed Glaessgen is the NASA Contract
Monitor. The simulations needed to complete this study were carried out
at NASA LaRC computing facilities.
NR 35
TC 21
Z9 21
U1 2
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0965-0393
J9 MODEL SIMUL MATER SC
JI Model. Simul. Mater. Sci. Eng.
PD JUN
PY 2010
VL 18
IS 4
AR 045004
DI 10.1088/0965-0393/18/4/045004
PG 33
WC Materials Science, Multidisciplinary; Physics, Applied
SC Materials Science; Physics
GA 588QF
UT WOS:000277087400004
ER
PT J
AU Furlanetto, SR
Stoever, SJ
AF Furlanetto, Steven R.
Stoever, Samuel Johnson
TI Secondary ionization and heating by fast electrons
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE atomic processes; intergalactic medium; diffuse radiation
ID DARK-MATTER DECAYS; 1ST BLACK-HOLES; 21 CM SIGNATURE; HIGH-REDSHIFT;
INTERGALACTIC MEDIUM; ENERGETIC PARTICLES; IMPACT IONIZATION; THERMAL
ELECTRONS; X-RAYS; REIONIZATION
AB We examine the fate of fast electrons (with energies E > 10 eV) in a thermal gas of primordial composition. To follow their interactions with the background gas, we construct a Monte Carlo model that includes: (1) electron-electron scattering (which transforms the electron kinetic energy into heat), (2) collisional ionization of hydrogen and helium (which produces secondary electrons that themselves scatter through the medium) and (3) collisional excitation (which produces secondary photons, whose fates we also follow approximately). For the last process, we explicitly include all transitions to upper levels n < 4, together with a well-motivated extrapolation to higher levels. In all cases, we use recent calculated cross-sections at E < 1 keV and the Bethe approximation to extrapolate to higher energies. We compute the fractions of energy deposited as heat, ionization (tracking H i and the helium species separately) and excitation (tracking H i Ly alpha separately) under a broad range of conditions appropriate to the intergalactic medium. The energy deposition fractions depend on both the background ionized fraction and the electron energy but are nearly independent of the background density. We find good agreement with some, but not all, previous calculations at high energies. Electronic tables of our results are available.
C1 [Furlanetto, Steven R.; Stoever, Samuel Johnson] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Furlanetto, Steven R.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94043 USA.
[Stoever, Samuel Johnson] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Furlanetto, SR (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
EM sfurlane@astro.ucla.edu
FU NSF [AST-0829737, PHY-0552500]; David and Lucile Packard Foundation;
NASA [NNA09DB30A]; UCLA
FX We thank M. Valdes for helpful comments. SRF was partially supported by
the NSF through grant AST-0829737, by the David and Lucile Packard
Foundation and by NASA through the LUNAR programme. The LUNAR consortium
(http://lunar.colorado.edu), headquartered at the University of
Colorado, is funded by the NASA Lunar Science Institute (via Cooperative
Agreement NNA09DB30A) to investigate concepts for astrophysical
observatories on the Moon. SJS was supported by a Research Experiences
for Undergraduates grant at UCLA, NSF PHY-0552500. We thank Agner Fog
for making a public version of the Mersenne Twister algorithm available
and Igor Bray and Yuri Ralchenko for making the CCC data base available
electronically.
NR 45
TC 51
Z9 51
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2010
VL 404
IS 4
BP 1869
EP 1878
DI 10.1111/j.1365-2966.2010.16401.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 600JG
UT WOS:000277981400017
ER
PT J
AU Braun, SA
AF Braun, Scott A.
TI Reevaluating the Role of the Saharan Air Layer in Atlantic Tropical
Cyclogenesis and Evolution
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID VERTICAL WIND SHEAR; AFRICAN EASTERLY JET; UPPER-TROPOSPHERIC TROUGHS;
PREDICTION SCHEME SHIPS; WATER-VAPOR RADIANCES; HURRICANE-BONNIE 1998;
NUMERICAL SIMULATIONS; WAVE DISTURBANCES; NORTH-ATLANTIC; INNER-CORE
AB The existence of the Saharan air layer (SAL), a layer of warm, dry, dusty air frequently present over the tropical Atlantic Ocean, has long been appreciated. The nature of its impacts on hurricanes remains unclear, with some researchers arguing that the SAL amplifies hurricane development and with others arguing that it inhibits it. The potential negative impacts of the SAL include 1) vertical wind shear associated with the African easterly jet: 2) warm air aloft, which increases thermodynamic stability at the base of the SAL; and 3) dry air, which produces cold downdrafts. Multiple NASA satellite datasets and NCEP global analyses are used to characterize the SAL's properties and evolution ill relation to tropical cyclones and to evaluate these potential negative influences. The SAL is shown to occur in a large-scale environment that is already characteristically dry as a result of large-scale subsidence. Strong surface heating and deep dry convective mixing enhance the dryness at low levels (primarily below similar to 700 hPa), but moisten the air at midlevels. Therefore, mid-to-upper-level dryness is not generally a defining characteristic of the SAL, but is instead often a signature of subsidence. The results further show that storms generally form on the southern side of the jet, where the background cyclonic vorticity is high. Based upon its depiction in NCEP Global Forecast System meteorological analyses, the jet often helps to form the northern side of the storms and is present to equal extents for both strengthening and weakening storms, suggesting that jet-induced vertical wind shear may not be a frequent negative influence. Warm SAL air is confined to regions north of the jet and generally does not impact the tropical cyclone precipitation south of the jet.
Composite analyses of the early stages of tropical cyclones occurring in association with the SAL support the inferences from the individual cases noted above. Furthermore, separate composites for strongly strengthening and for weakening storms show few substantial differences in the SAL characteristics between these two groups, suggesting that the SAL is not a determinant of whether a storm will intensify or weaken in the days after formation. Key differences between these cases are found mainly at upper levels where the flow over strengthening storms allows for an expansive outflow and produces little vertical shear, while for weakening storms, the shear is stronger and the outflow is significantly constrained.
C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Braun, SA (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-1, Greenbelt, MD 20771 USA.
EM scott.a.braun@nasa.gov
FU NASA
FX The authors thank Karen Mohr and Ron McTaggart-Cowan for their helpful
comments on the manuscript. This work was supported by Dr. Ramesh Kakar
at NASA Headquarters with funds from the NASA Hurricane Science Research
Program.
NR 87
TC 46
Z9 47
U1 3
U2 16
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 JUN
PY 2010
VL 138
IS 6
BP 2007
EP 2037
DI 10.1175/2009MWR3135.1
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 622QE
UT WOS:000279677500002
ER
PT J
AU Bleck, R
Benjamin, S
Lee, J
MacDonald, AE
AF Bleck, Rainer
Benjamin, Stan
Lee, Jin
MacDonald, Alexander E.
TI On the Use of an Adaptive, Hybrid-Isentropic Vertical Coordinate in
Global Atmospheric Modeling
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID SHALLOW-WATER EQUATIONS; WEATHER PREDICTION; SIGMA MODEL; NUMERICAL
INVESTIGATIONS; DIFFERENCE SCHEME; SIMULATION; SYSTEMS
AB This article is one in a series describing the functionality of the Flow-Following, Finite-Volume Icosahedral Model (FIM) developed at NOAA's Earth System Research Laboratory. Emphasis in this article is on the design of the vertical coordinate-the "flow following" aspect of FIM. The coordinate is terrain-following near the ground and isentropic in the free atmosphere. The spatial transition between the two coordinates is adaptive and is based on the arbitrary Lagrangian-Eulerian (ALE) paradigm. The impact of vertical resolution trade-offs between the present hybrid approach and traditional terrain-following coordinates is demonstrated in a three-part case study.
C1 [Bleck, Rainer] NOAA, ESRL, Global Syst Div, Boulder, CO 80303 USA.
[Bleck, Rainer] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
RP Bleck, R (reprint author), NOAA, ESRL, Global Syst Div, 325 Broadway, Boulder, CO 80303 USA.
EM rainer.bleck@noaa.gov
RI Bleck, Rainer/C-6417-2015; Benjamin, Stan/C-5818-2015; Lee,
JIN-LUEN/G-5364-2015
OI Benjamin, Stan/0000-0002-5751-8236;
NR 47
TC 13
Z9 13
U1 1
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD JUN
PY 2010
VL 138
IS 6
BP 2188
EP 2210
DI 10.1175/2009MWR3103.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 622QE
UT WOS:000279677500011
ER
PT J
AU Kaul, AB
Yang, EH
AF Kaul, Anupama B.
Yang, Eui-Hyeok
TI A Special Issue on Nanoscale Materials, Structures and Devices for
Sensors and Systems Applications
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Editorial Material
C1 [Kaul, Anupama B.] CALTECH, Jet Prop Labs, Pasadena, CA 91125 USA.
[Yang, Eui-Hyeok] Stevens Inst Technol, Dept Mech Engn, Hoboken, NJ 07030 USA.
[Kaul, Anupama B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Yang, Eui-Hyeok] Stevens Inst Technol, Multiuser Micro Device Lab MDL, Hoboken, NJ 07030 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Labs, Pasadena, CA 91125 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER SCIENTIFIC PUBLISHERS
PI STEVENSON RANCH
PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA
SN 1941-4900
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD JUN
PY 2010
VL 2
IS 2
SI SI
BP 63
EP 64
DI 10.1166/nnl.2010.1061
PG 2
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MH
UT WOS:000293210900001
ER
PT J
AU Son, KA
Liao, AN
Lung, G
Gallegos, M
Hatake, T
Harris, RD
Scheick, LZ
Smythe, WD
AF Son, Kyung-ah
Liao, Anna
Lung, Gerald
Gallegos, Manuel
Hatake, Toshiro
Harris, Richard D.
Scheick, Leif Z.
Smythe, William D.
TI GaN-Based High Temperature and Radiation-Hard Electronics for Harsh
Environments
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Article
DE AlGaN/GaN; MOS Transistor; Schottky-Free; High Temperature;
Radiation-Hard
ID FIELD-EFFECT TRANSISTORS; MOBILITY TRANSISTORS; HYDROSTATIC-PRESSURE;
ALGAN/GAN HEMTS; DEPENDENCE; DC; DEVICES
AB We develop novel GaN-based high temperature and radiation-hard electronics to realize data acquisition electronics and transmitters suitable for operations in harsh planetary environments. In this paper, we discuss our research on AlGaN/GaN metal-oxide-semiconductor (MOS) transistors that are targeted for 500 degrees C operation and > 2 Mrad radiation hardness. For the target device performance, we develop Schottky-free AlGaN/GaN MOS transistors, where a gate electrode is processed in a MOS layout using an Al(2)O(3) gate dielectric layer. The AlGaN/GaN MOS transistors fabricated with the wide-bandgap gate oxide layer enable Schottky-free gate electrodes, resulting in a much reduced gate leakage current and an improved sub-threshold current than the current AlGaN/GaN field effect transistors. In this study, characterization of our AlGaN/GaN MOS transistors is carried out over the temperature range of 25 degrees C to 500 degrees C. The I(ds)-V(gs) and I(ds)-V(gs) curves measured as a function of temperature show an excellent pinch-off behavior up to 450 degrees C. Off-state degradation is not observed up to 400 degrees C, but it becomes measurable at 450 degrees C. The off-state current is increased at 500 degrees C due to the gate leakage current, and the AlGaN/GaN MOS HEMT does not get pinched-off completely. Radiation hardness testing of the AlGaN/GaN MOS transistors is performed using a 50 MeV (60)Co gamma source to explore effects of TID (total ion dose). Excellent I(ds)-V(gs), and I(ds)-V(gs) characteristics are measured even after exposures to a TID of 2 Mrad. A slight decrease of saturation current (Delta I(dss) similar to 3 mA/mm) is observed due to the 2 Mrad irradiation.
C1 [Son, Kyung-ah; Liao, Anna; Lung, Gerald; Gallegos, Manuel; Hatake, Toshiro; Harris, Richard D.; Scheick, Leif Z.; Smythe, William D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Son, KA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 21
TC 6
Z9 6
U1 1
U2 10
PU AMER SCIENTIFIC PUBLISHERS
PI STEVENSON RANCH
PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA
SN 1941-4900
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD JUN
PY 2010
VL 2
IS 2
SI SI
BP 89
EP 95
DI 10.1166/nnl.2010.1063
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MH
UT WOS:000293210900006
ER
PT J
AU Prokopuk, N
Son, KA
Waltz, C
AF Prokopuk, Nicholas
Son, Kyung-Ah
Waltz, Chad
TI Free Standing Nanocrossbar Arrays with Molecular Throughput
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Article
DE Electron Tunneling; Nanogap; Chemical Etch
ID MONOLAYER/TI DEVICES; NANOGAP ELECTRODES; VAPOR-DEPOSITION; FABRICATION;
TI; PATHWAYS; CIRCUITS; SURFACES; GLASSES; SWITCH
AB We report a new approach for fabricating vacant nanocrossbar arrays using a combination of lithography and selective chemical etch. Two parallel arrays of gold wires are lithographically patterned orthogonal to each other with a chromium layer (2-5 nm thick) sandwiched between the wire arrays. A silicon oxide mesh is sputtered over the metal ensemble leaving the crossing points free of the oxide layer. The chromium layer is subsequently removed via selective chemical etch leaving a gold architecture with vertical separations that are on the order of a few nanometers. The silicon oxide mesh anchors the gold wires in place creating a robust nanoarchitecture. The nanogaps can be filled with fluids resulting in a change of the junction's resistance. The variability in the vertical separations between the wires within an array is only a few Angstroms. These results demonstrate that molecular-sized gaps can be created without the use of a molecular template.
C1 [Prokopuk, Nicholas; Waltz, Chad] NAVAIR Res Dept, Chem Branch, China Lake, CA 93555 USA.
[Son, Kyung-Ah] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Prokopuk, N (reprint author), NAVAIR Res Dept, Chem Branch, China Lake, CA 93555 USA.
FU NAWCWD, China Lake; National Aeronautics and Space Administration
FX Nicholas Prokopuk thanks the Defense Threat Reduction Agency for
funding. This work was partially supported by the Independent Applied
Research Program at NAWCWD, China Lake under the sponsorship of ONR. The
research in this paper was carried out partly at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 30
TC 0
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U1 0
U2 3
PU AMER SCIENTIFIC PUBLISHERS
PI VALENCIA
PA 26650 THE OLD RD, STE 208, VALENCIA, CA 91381-0751 USA
SN 1941-4900
EI 1941-4919
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD JUN
PY 2010
VL 2
IS 2
SI SI
BP 96
EP 101
DI 10.1166/nnl.2010.1064
PG 6
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MH
UT WOS:000293210900007
ER
PT J
AU Kaul, AB
Khan, AR
Megerian, KG
Epp, L
Bagge, L
Jennings, AT
Jang, D
Greer, JR
AF Kaul, A. B.
Khan, A. R.
Megerian, K. G.
Epp, L.
Bagge, L.
Jennings, A. T.
Jang, D.
Greer, J. R.
TI Nano-Electro-Mechanical Switches Derived from Carbon-Based Nanomaterials
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Article
DE Nanoelectronics; NEMS; Mechanical Resonators; SWNTs; CNFs; In Situ
Characterization
ID NANOFIBERS
AB We provide an overview of our work where carbon-based nanostructures have been applied to two-dimensional (2D) planar and three-dimensional (3D) vertically-oriented nano-electro-mechanical (NEM) switches. In the first configuration, laterally oriented single-walled nanotubes (SWNTs) synthesized using thermal chemical vapor deposition (CVD) were implemented for forming bridge-type 2D NEMS switches, where switching voltages were on the order of a few volts. In the second configuration, vertically oriented carbon nanofibers (CNFs) synthesized using plasma-enhanced (PE) CVD have been explored for their potential application in 3D NEMS. We have performed nanomechanical measurements on such vertically oriented tubes using nanoindentation to determine the mechanical robustness of the CNFs. Electrostatic switching was demonstrated in the CNFs synthesized on refractory metallic nitride substrates, where a nanoprobe was used as the actuating electrode inside a scanning-electron-microscope. The switching voltages were determined to be in the tens of volts range and van der Waals interactions at these length scales appeared significant, suggesting such structures are promising for nonvolatile memory applications. A finite element model was also developed to determine a theoretical pull-in voltage which was compared to experimental results.
C1 [Kaul, A. B.; Khan, A. R.; Megerian, K. G.; Epp, L.; Bagge, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jennings, A. T.; Jang, D.; Greer, J. R.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Jang, Dongchan/C-9510-2012
OI Jang, Dongchan/0000-0002-2814-9734
FU National Aeronautics and Space Administration; internal Research and
Technology Development (RTD) program
FX We sincerely acknowledge Robert Kowalczyk for his assistance with the
PECVD growth chamber and performing chamber upgrades as necessary, in
addition to Dr. Choonsup Lee, Dr. Richard L. Baron and Dr. Paul von
Allmen for useful discussions. We would also like to thank Shelby
Hutchens of the California Institute of Technology (Caltech) and Brian
Peters of Agilent Technologies for the images taken in Figures 2(a) and
(b). We gratefully acknowledge critical support and infrastructure
provided for this work by the Kavli Nanoscience Institute at Caltech.
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 through the internal
Research and Technology Development (R&TD) program.
NR 21
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U1 0
U2 11
PU AMER SCIENTIFIC PUBLISHERS
PI STEVENSON RANCH
PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA
SN 1941-4900
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD JUN
PY 2010
VL 2
IS 2
SI SI
BP 163
EP 169
DI 10.1166/nnl.2010.1076
PG 7
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MH
UT WOS:000293210900017
ER
PT J
AU Kaul, AB
Megerian, KG
Bagge, L
Epp, L
LeDuc, HG
Coles, JB
Eastwood, M
Green, RO
Foote, M
AF Kaul, A. B.
Megerian, K. G.
Bagge, L.
Epp, L.
LeDuc, H. G.
Coles, J. B.
Eastwood, M.
Green, R. O.
Foote, M.
TI Carbon Nanomaterials for Nanoelectronics and Optical Applications
SO NANOSCIENCE AND NANOTECHNOLOGY LETTERS
LA English
DT Article
DE Nano-Sensors; Pressure Sensors; Resonators; NEMS; Optical Absorbers;
Black Bodies
ID SWITCHES
AB Carbon-based nanomaterials have been actively applied to a diverse array of space-based applications in electronics and optics at the Jet Propulsion Laboratory. In the area of nano-electromechanical-systems (NEMS), we describe the implementation of carbon nanotubes (CNTs) and carbon nanofibers (CNFs) to dc nanorelays, as well as for AC resonator applications, which are under consideration for extreme environment electronics. We have also implemented single-walled nanotubes (SWNTs) to physical sensing, specifically for forming miniaturized pressure sensors for vacuum micro-cavity applications, where the mechanism of operation in such sensors relies on the thermal conductivity principle. Finally, we have also initiated an effort to apply arrays of vertically oriented CNTs for optical applications, specifically as broad-band optical absorbers, potentially for calibration targets. In this paper, we provide an overview of the recent results in the three application areas of carbon nanomaterials.
C1 [Kaul, A. B.; Megerian, K. G.; Bagge, L.; Epp, L.; LeDuc, H. G.; Coles, J. B.; Eastwood, M.; Green, R. O.; Foote, M.] 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.
FU National Aeronautics and Space Administration; internal Research and
Technology Development (RTD) program
FX We would like to thank Robert Kowalczyk for making system modifications
to the dc PECVD growth chamber, Choonsup Lee, Richard Baron and Paul von
Allmen for useful discussions. 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 through the internal Research and Technology Development (R&TD)
program.
NR 16
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U1 0
U2 8
PU AMER SCIENTIFIC PUBLISHERS
PI STEVENSON RANCH
PA 25650 NORTH LEWIS WAY, STEVENSON RANCH, CA 91381-1439 USA
SN 1941-4900
J9 NANOSCI NANOTECH LET
JI Nanosci. Nanotechnol. Lett.
PD JUN
PY 2010
VL 2
IS 2
SI SI
BP 170
EP 174
DI 10.1166/nnl.2010.1077
PG 5
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 798MH
UT WOS:000293210900018
ER
PT J
AU Johnson, SW
Thedinga, JF
Neff, AD
Harris, PM
Lindeberg, MR
Maselko, JM
Rice, SD
AF Johnson, Scott W.
Thedinga, John F.
Neff, A. Darcie
Harris, Patricia M.
Lindeberg, Mandy R.
Maselko, Jacek M.
Rice, Stanley D.
TI Fish Assemblages in Nearshore Habitats of Prince William Sound, Alaska
SO NORTHWEST SCIENCE
LA English
DT Article
ID VALDEZ OIL-SPILL; SHALLOW-WATER HABITATS; LIFE-HISTORY; REPRODUCTIVE
SUCCESS; SOUTHEASTERN ALASKA; CLUPEA-PALLASI; NORTHERN GULF; PACIFIC;
COMMUNITIES; ABUNDANCE
AB We sampled fish at eight locations in western Prince William Sound (PWS), Alaska, in April, July, and September 2006, and July 2007, to identify species assemblages and habitat use. At each location, fish were sampled with a 37-m long variable mesh beach seine in three nearshore habitats: bedrock outcrops, eelgrass meadows, and cobble beaches with kelp. A total of 49,060 fish representing 45 species were captured in 95 beach seine hauls. Catch-per-unit-effort (CPUE, all species) did not differ by season but did differ by habitat type CPUE was greater in eelgrass and kelp than in bedrock. Seasonal pulses in catch were evident for some species; pink salmon were captured only in spring and summer, Pacific herring only in summer and fall, and capelin only in fall. Species richness was greater in summer (34) than in spring (23) or fall (28), and greater in eelgrass (34) than in bedrock (22) or kelp (33). Species that were good discriminators among seasonal collections were pink salmon, saffron cod, crescent gunnel, and Pacific herring, whereas species that were good discriminators among habitat collections were crescent gunnel, tubesnout, bay pipefish, saffron cod, and Arctic shanny. Of the most abundant species captured, most were juveniles based on estimated size at maturity. The summer fish assemblage in western PWS has changed over the last 20 years, especially with the appearance in large numbers of saffron cod. Sites in this study can be monitored periodically to track future changes in fish assemblages and habitat that may result from local and regional human disturbance.
C1 [Johnson, Scott W.; Thedinga, John F.; Neff, A. Darcie; Harris, Patricia M.; Lindeberg, Mandy R.; Maselko, Jacek M.; Rice, Stanley D.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA.
RP Johnson, SW (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA.
EM scott.johnson@noaa.gov
FU North Pacific Research Board [249]; NOAA
FX We thank the crews of the RV Solstice and RV Pandalus for their
invaluable support at sea. We would especially like to thank Matthew
Eagleton of the NMFS regional office in Anchorage for providing
logistical support. We also thank Dugan Greenwell. Kris Holderied, John
Hudson, Sarah Lyn McConahay, John Moran, Sue Saupe, Fletcher Sewall, and
Ash win Sreenivasan for help with field and laboratory work. Funding for
this research was provided by the North Pacific Research Board
(Publication 249) and the NOAA Fisheries Essential Fish Habitat Program.
Reference to trade names does not imply endorsement by the National
Marine Fisheries Service, NOAA.
NR 44
TC 5
Z9 5
U1 5
U2 21
PU WASHINGTON STATE UNIV
PI PULLMAN
PA PO BOX 645020, PULLMAN, WA 99164-5910 USA
SN 0029-344X
J9 NORTHWEST SCI
JI Northwest Sci.
PD SUM
PY 2010
VL 84
IS 3
BP 266
EP 280
PG 15
WC Ecology
SC Environmental Sciences & Ecology
GA 652VU
UT WOS:000282039700006
ER
PT J
AU VanZwieten, JH
Driscoll, FR
VanZwieten, TS
Marikle, SP
AF VanZwieten, J. H., Jr.
Driscoll, F. R.
VanZwieten, T. S.
Marikle, S. P.
TI Development of an adaptive disturbance rejection system for the rapidly
deployable stable platform-part 1: Mathematical modeling and open loop
response
SO OCEAN ENGINEERING
LA English
DT Article
DE RDSP; RDSC; Spar; Simulation; Sea base; Wave disturbances; Load
disturbances; Open loop response; Seakeeping; Crane ship
AB A Rapidly Deployable Stable Platform (RDSP) concept was investigated at Florida Atlantic University in response to military and civilian needs for ocean platforms with improved sea-keeping characteristics. The RDSP is designed to have enhanced sea-keeping abilities through the combination of a novel hull and thruster design coupled with active control. The RDSP is comprised of a catamaran that attaches via a hinge to a spar, enabling it to transit like a trimaran and then reconfigure so that the spar lifts the catamaran out of the water, creating a stable spar platform. The focus of this research is the mathematical modeling, simulation, and response characterization of the RDSP to provide a foundation for controller design, testing, and tuning. The mathematical model includes a detailed representation of residual drag, friction drag, added mass, hydrostatic and hydrodynamic pressure, and control actuator dynamics. Validation has been performed by comparing the simulation predicted motions of the RDSP operating in waves to the measured motions of the 1/10th scale prototype measured at sea. Resulting from this paper is an empirical assessment of the response characteristics of the RDSP that quantifies the performance under extreme conditions and provides a solid basis for controller development and testing. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [VanZwieten, J. H., Jr.] Florida Atlantic Univ, Ctr Ocean Energy Technol, Dania, FL 33004 USA.
[Driscoll, F. R.; Marikle, S. P.] Florida Atlantic Univ, Dept Ocean & Mech Engn, Dania, FL 33004 USA.
[VanZwieten, T. S.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP VanZwieten, JH (reprint author), Florida Atlantic Univ, Ctr Ocean Energy Technol, 101 N Beach Rd, Dania, FL 33004 USA.
EM jvanzwi@fau.edu
FU Office of Naval Research [N00014-06-1-0461]
FX The authors gratefully acknowledge the Office of Naval Research, code
33, program manager Kelly Cooper for funding this work under grant
N00014-06-1-0461. The authors would also like to thank FAU's senior
design class of 2005 for developing and assembling the original 1/10th
scale prototype RDSP, which was modified to produce the RDSP prototype
used to validate the simulation presented in this paper.
NR 18
TC 2
Z9 3
U1 2
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0029-8018
J9 OCEAN ENG
JI Ocean Eng.
PD JUN
PY 2010
VL 37
IS 8-9
BP 833
EP 846
DI 10.1016/j.oceaneng.2010.02.014
PG 14
WC Engineering, Marine; Engineering, Civil; Engineering, Ocean;
Oceanography
SC Engineering; Oceanography
GA 605OA
UT WOS:000278355700016
ER
PT J
AU Weber, AL
AF Weber, Arthur L.
TI Sugar-Driven Prebiotic Synthesis of Ammonia from Nitrite
SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES
LA English
DT Article
DE Ammonia synthesis; Nitrite; Reduction; Sugar chemistry; Ferric;
Prebiotic synthesis; Origin of life
ID MILD AQUEOUS CONDITIONS; ACID SYNTHESIS; DISPROPORTIONATION;
TRANSFORMATIONS; FORMALDEHYDE; METABOLISM; REDUCTION; ORIGIN; MODEL;
LIFE
AB Reaction of 3-5 carbon sugars, glycolaldehyde, and alpha-ketoaldehydes with nitrite under mild anaerobic aqueous conditions yielded ammonia, an essential substrate for the synthesis of nitrogen-containing molecules during abiogenesis. Under the same conditions, ammonia synthesis was not driven by formaldehyde, glyoxylate, 2-deoxyribose, and glucose, a result indicating that the reduction process requires an organic reductant containing either an accessible alpha-hydroxycarbonyl group or an alpha-dicarbonyl group. Small amounts of aqueous Fe(+3) catalyzed the sugar-driven synthesis of ammonia. The glyceraldehyde concentration dependence of ammonia synthesis, and control studies of ammonia's reaction with glyceraldehyde, indicated that ammonia formation is accompanied by incorporation of part of the synthesized ammonia into sugar-derived organic products. The ability of sugars to drive the synthesis of ammonia is considered important to abiogenesis because it provides a way to generate photochemically unstable ammonia at sites of sugar-based origin-of-life processes from nitrite, a plausible prebiotic nitrogen species.
C1 NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Weber, AL (reprint author), NASA, SETI Inst, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA.
EM arthur.l.weber@nasa.gov
FU Exobiology Program of the National Aeronautics and Space Administration
[NNX08AP48A]
FX I thank Esther Varon for technical assistance in these studies. This
investigation was supported by a grant (NNX08AP48A) from the Exobiology
Program of the National Aeronautics and Space Administration.
NR 21
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U1 2
U2 8
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 JUN
PY 2010
VL 40
IS 3
BP 245
EP 252
DI 10.1007/s11084-010-9208-z
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 587WY
UT WOS:000277028000001
PM 20213158
ER
PT J
AU Kruger, H
Dikarev, V
Anweiler, B
Dermott, SF
Graps, AL
Grun, E
Gustafson, BA
Hamilton, DP
Hanner, MS
Horanyi, M
Kissel, J
Linkert, D
Linkert, G
Mann, I
McDonnell, JAM
Morfill, GE
Polanskey, C
Schwehm, G
Srama, R
AF Krueger, H.
Dikarev, V.
Anweiler, B.
Dermott, S. F.
Graps, A. L.
Gruen, E.
Gustafson, B. A.
Hamilton, D. P.
Hanner, M. S.
Horanyi, M.
Kissel, J.
Linkert, D.
Linkert, G.
Mann, I.
McDonnell, J. A. M.
Morfill, G. E.
Polanskey, C.
Schwehm, G.
Srama, R.
TI Three years of Ulysses dust data: 2005 to 2007
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Interstellar dust; Interplanetary dust; Dust dynamics; Interstellar
medium; Dust in-situ measurements
ID INTERSTELLAR NEUTRAL HELIUM; INNER SOLAR-SYSTEM; JOVIAN SYSTEM;
METEOROID ENVIRONMENT; KINETIC-PARAMETERS; RADIATION PRESSURE;
MASS-DISTRIBUTION; ASTEROID BELT; 1 AU; GALILEO
AB The Ulysses spacecraft has been orbiting the Sun on a highly inclined ellipse (i = 79 degrees, perihelion distance 1.3 AU, aphelion distance 5.4 AU) since it encountered Jupiter in February 1992. Since then it has made almost three revolutions about the Sun. Here we report on the final three years of data taken by the on-board dust detector. During this time, the dust detector recorded 609 dust impacts of particles with masses 10(-16) g <= m <= 10(-7) g, bringing the mission total to 6719 dust data sets. The impact rate varied from a low value of 0.3 per day at high ecliptic latitudes to 1.5 per day in the inner solar system. The impact direction of the majority of impacts between 2005 and 2007 is compatible with particles of interstellar origin; the rest are most likely interplanetary particles. We compare the interstellar dust measurements from 2005/2006 with the data obtained during earlier periods (1993/1994) and (1999/2000) when Ulysses was traversing the same spatial region at southern ecliptic latitudes but the solar cycle was at a different phase. During these three intervals the impact rate of interstellar grains varied by more than a factor of two. Furthermore, in the two earlier periods the grain impact direction was in agreement with the flow direction of the interstellar helium while in 2005/2006 we observed a shift in the approach direction of the grains by approximately 30 away from the ecliptic plane. The reason for this shift remains unclear but may be connected with the configuration of the interplanetary magnetic field during solar maximum. We also find that the dust measurements are in agreement with the interplanetary flux model of Staubach et al. (1997) which was developed to fit a 5-year span of Ulysses data. (C) 2009 Elsevier Ltd. All rights reserved.
C1 [Krueger, H.; Kissel, J.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Krueger, H.; Anweiler, B.; Gruen, E.; Linkert, D.; Linkert, G.; Srama, R.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Dikarev, V.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany.
[Dermott, S. F.; Gustafson, B. A.] Univ Florida, SSRB 211, Gainesville, FL 32609 USA.
[Graps, A. L.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Gruen, E.; Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hamilton, D. P.] Univ Maryland, College Pk, MD 20742 USA.
[Hanner, M. S.] Univ Massachusetts, Dept Astron, LGRT 619, Amherst, MA 01003 USA.
[Mann, I.] Kinki Univ, Sch Sci & Engn, Osaka 5778502, Japan.
[McDonnell, J. A. M.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Morfill, G. E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Polanskey, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schwehm, G.] ESAC, Villanueva De La Canada 28691, Spain.
[Srama, R.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany.
RP Kruger, H (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
EM krueger@mps.mpg.de
OI Horanyi, Mihaly/0000-0002-5920-9226
FU Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR) [50 ON 9107, 50 QJ
9503]; Max-Planck-Institut fur Kernphysik; Max-Planck-Institut fur
Sonnensys-temforschung
FX We dedicate this work to the memory of Dietmar Linkert who passed away
in spring 2009. He was Principal Engineer for space instruments at MPI
fur Kernphysik including the dust instruments flown on the HEOS-2,
Helios, Galileo, Ulysses and Cassini missions. His friends and
colleagues around the world appreciated his experience and sought his
professional advice. We thank the Ulysses project at ESA and NASA/JPL
for effective and successful mission operations. This work has been
supported by the Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR)
under Grants 50 ON 9107 and 50 QJ 9503. Support by Max-Planck-Institut
fur Kernphysik and Max-Planck-Institut fur Sonnensys-temforschung is
also gratefully acknowledged. The authors also wish to thank two
anonymous referees for their valuable comments for the manuscript.
NR 73
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U1 1
U2 10
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 JUN
PY 2010
VL 58
IS 7-8
BP 951
EP 964
DI 10.1016/j.pss.2009.11.002
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 612XN
UT WOS:000278939200001
ER
PT J
AU Kruger, H
Bindschadler, D
Dermott, SF
Graps, AL
Grun, E
Gustafson, BA
Hamilton, DP
Hanner, MS
Horanyi, M
Kissel, J
Linkert, D
Linkert, G
Mann, I
McDonnell, JAM
Moissl, R
Morfill, GE
Polanskey, C
Roy, M
Schwehm, G
Srama, R
AF Krueger, H.
Bindschadler, D.
Dermott, S. F.
Graps, A. L.
Gruen, E.
Gustafson, B. A.
Hamilton, D. P.
Hanner, M. S.
Horanyi, M.
Kissel, J.
Linkert, D.
Linkert, G.
Mann, I.
McDonnell, J. A. M.
Moissl, R.
Morfill, G. E.
Polanskey, C.
Roy, M.
Schwehm, G.
Srama, R.
TI Galileo dust data from the jovian system: 2000 to 2003
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Circumplanetary dust; Planetary rings; Dust/magnetosphere interaction;
Interplanetary dust; Dusty plasmas
ID JUPITERS GOSSAMER RINGS; PLANETARY SATELLITES; INTERSTELLAR DUST; STREAM
PARTICLES; ULYSSES; IO; MAGNETOSPHERE; INTERPLANETARY; DETECTOR; CLOUDS
AB The Galileo spacecraft was the first man-made satellite of Jupiter, orbiting the planet between December 1995 and September 2003. The spacecraft was equipped with a highly sensitive dust detector that monitored the jovian dust environment between approximately 2 and 370 R(J) (jovian radius R(J)=71 492 km). The Galileo dust detector was a twin of the one flying on board the Ulysses spacecraft. This is the tenth in a series of papers dedicated to presenting Galileo and Ulysses dust data. Here we present data from the Galileo dust instrument for the period January 2000 to September 2003 until Galileo was destroyed in a planned impact with Jupiter. The previous Galileo dust data set contains data of 2883 particles detected during Galileo's interplanetary cruise and 12 978 particles detected in the jovian system between 1996 and 1999. In this paper we report on the data of additional 5389 particles measured between 2000 and the end of the mission in 2003. The majority of the 21 250 particles for which the full set of measured impact parameters (impact time, impact direction, charge rise times, charge amplitudes, etc.) was transmitted to Earth were tiny grains (about 10 nm in radius), most of them originating from Jupiter's innermost Galilean moon lo. They were detected throughout the jovian system and the impact rates frequently exceeded 10 min(-1). Surprisingly large impact rates up to 100 min(-1) occurred in August/September 2000 when Galileo was far away (approximate to 280 R(J)) from Jupiter, implying dust ejection rates in excess of 100 kg s(-1). This peak in dust emission appears to coincide with strong changes in the release of neutral gas from the lo torus. Strong variability in the lo dust flux was measured on timescales of days to weeks, indicating large variations in the dust release from lo or the lo torus or both on such short timescales. Galileo has detected a large number of bigger micron-sized particles mostly in the region between the Galilean moons. A surprisingly large number of such bigger grains was measured in March 2003 within a four-day interval when Galileo was outside Jupiter's magnetosphere at approximately 350 R(J) jovicentric distance. Two passages of Jupiter's gossamer rings in 2002 and 2003 provided the first actual comparison of in-situ dust data from a planetary ring with the results inferred from inverting optical images. Strong electronics degradation of the dust instrument due to the harsh radiation environment of Jupiter led to increased calibration uncertainties of the dust data. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [Krueger, H.; Kissel, J.; Moissl, R.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Krueger, H.; Gruen, E.; Linkert, D.; Linkert, G.; Srama, R.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Bindschadler, D.; Polanskey, C.; Roy, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dermott, S. F.; Gustafson, B. A.] Univ Florida, SSRB 211, Gainesville, FL 32609 USA.
[Graps, A. L.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Gruen, E.; Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hamilton, D. P.] Univ Maryland, College Pk, MD 20742 USA.
[Hanner, M. S.] Univ Massachusetts, Astron Dept LGRT 619, Amherst, MA 01003 USA.
[Mann, I.] Kinki Univ, Sch Sci & Engn, Osaka 5778502, Japan.
[McDonnell, J. A. M.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[Morfill, G. E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Schwehm, G.] ESAC, Villanueva De La Canada 28691, Spain.
[Srama, R.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany.
RP Kruger, H (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
EM krueger@mps.mpg.de
OI Horanyi, Mihaly/0000-0002-5920-9226
FU German Bundesministerium fur Bildung und Forschung through Deutsches
Zentrum fur Luft- und Raumfahrt e.V. (DLR) [50 QJ 9503 3]; MPI fur
Kernphysik; MPI fur Sonnensystemforschung
FX We dedicate this work to the memory of Dietmar Linkert who passed away
in spring 2009. He was Principal Engineer for space instruments at MPI
fur Kernphysik including the dust instruments flown on the HEOS-2,
Helios, Galileo, Ulysses and Cassini missions. His friends and
colleagues around the world appreciated his experience and sought his
professional advice. The authors wish to thank the Galileo project at
NASA/JPL for effective and successful mission operations. This research
was supported by the German Bundesministerium fur Bildung und Forschung
through Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR, grant 50 QJ
9503 3). Support by MPI fur Kernphysik and MPI fur Sonnensystemforschung
is also gratefully acknowledged. The authors also wish to thank two
anonymous referees for their valuable comments for the manuscript.
NR 68
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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 JUN
PY 2010
VL 58
IS 7-8
BP 965
EP 993
DI 10.1016/j.pss.2010.03.003
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 612XN
UT WOS:000278939200002
ER
PT J
AU ten Kate, IL
Cardiff, EH
Dworkin, JP
Feng, SH
Holmes, V
Malespin, C
Stern, JG
Swindle, TD
Glavin, DP
AF ten Kate, I. L.
Cardiff, E. H.
Dworkin, J. P.
Feng, S. H.
Holmes, V.
Malespin, C.
Stern, J. G.
Swindle, T. D.
Glavin, D. P.
TI VAPoR - Volatile Analysis by Pyrolysis of Regolith - an instrument for
in situ detection of water, noble gases, and organics on the Moon
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Evolved Gas Analysis; Lunar Regolith; Lunar Volatiles; Mass
Spectrometer; Lunar Water Ice
ID LUNAR TRANSIENT PHENOMENA; LATE HEAVY BOMBARDMENT; CARBONACEOUS
CHONDRITES; MURCHISON METEORITE; MARS; APOLLO-16; NITROGEN; SUPPORT;
SCIENCE; SURFACE
AB We present the Volatile Analysis by Pyrolysis of Regolith (VAPoR) instrument design and demonstrate the validity of an in situ pyrolysis mass spectrometer for evolved gas analyses of lunar and planetary regolith samples. In situ evolved gas analyses of the lunar regolith have not yet been carried out and no atmospheric or evolved gas measurements have been made at the lunar poles. VAPoR is designed to do both kinds of measurements, is currently under development at NASA's Goddard Space Flight Center, and will be able to heat powdered regolith samples or rock drill fines up to 1400 degrees C in vacuo. To validate the instrument concept, evolved gas species released from different planetary analogs were determined as a function of temperature using a laboratory breadboard. Evolved gas measurements of an Apollo 16 regolith sample and a fragment of the carbonaceous meteorite Murchison were made by VAPoR and our results compared with existing data. The results imply that in situ evolved gas measurements of the lunar regolith at the polar regions by VAPoR will be a very powerful tool for identifying water and other volatile signatures of lunar or exogenous origin as potential resources for future human exploration. (C) 2010 Elsevier Ltd. All rights reserved.
C1 [ten Kate, I. L.; Cardiff, E. H.; Dworkin, J. P.; Feng, S. H.; Holmes, V.; Glavin, D. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[ten Kate, I. L.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA.
[Holmes, V.] Bast Technol, Lanham, MD 20706 USA.
[Malespin, C.] Auburn Univ Phys, Allison Labs 206, Auburn, AL 36849 USA.
[Stern, J. G.] Georgia Inst Technol, Dept Biol, Atlanta, GA 30332 USA.
[Swindle, T. D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP ten Kate, IL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Inge.L.tenKate@NASA.gov
RI Malespin, Charles/F-3445-2012; Glavin, Daniel/D-6194-2012; Dworkin,
Jason/C-9417-2012; Stern, Joshua/A-2691-2010
OI Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997;
Stern, Joshua/0000-0003-0626-5467
FU NASA [06-LSSO06-0002, 07-ASTID07-0020]; Goddard Internal Research and
Development
FX The authors thank P. Lowman, T. McCoy, L. Welzenbach, and G. Lofgren for
the samples used in this study. The authors also thank Marvin Noreiga
and the late Bob Abell for their invaluable help in keeping the VAPoR
instrument running, Geronimo Villanueva for his help with the 1DL code
used to analyze the data, and Bart Hendriks and Douwe van Hinsbergen for
their geological discussions. We also recognize the NASA Lunar Sortie
Science Opportunities (grant #06-LSSO06-0002) and Astrobiology Science
and Technology Instrument Development (grant #07-ASTID07-0020) programs,
Goddard Internal Research and Development funding for supporting this
research.
NR 54
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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 JUN
PY 2010
VL 58
IS 7-8
BP 1007
EP 1017
DI 10.1016/j.pss.2010.03.006
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 612XN
UT WOS:000278939200004
ER
PT J
AU Colavita, MM
AF Colavita, M. M.
TI Simultaneous Water Vapor and Dry Air Path Length Measurements with the
Keck Interferometer Nuller
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID PALOMAR TESTBED INTERFEROMETER; OUTER SCALES; MT WILSON; TURBULENCE;
SPECTRA; DELAY; VLTI; MIDI
AB K-band phase and group delay measurements of atmospheric turbulence are used as part of the Keck Interferometer nuller cophasing system to provide high-bandwidth path length compensation at N band. Because of atmospheric dispersion, the path length fluctuations from dry air and water vapor must be estimated separately, and the computation of the N-band feedforward quantities from the K-band measurements is described. Simultaneous K and N-band sky data are presented that show good correspondence with the underlying atmospheric models. Simultaneous power spectra of dry air and water vapor path length turbulence measured on an 85 m baseline with the Keck Interferometer over 44 nights between 2007 June and 2009 July are also presented. From the median power spectra, the rms path length fluctuations at K band from water vapor are found to be 48 times smaller than those for dry air, and the absolute level of the water vapor path length fluctuations is found to be a factor of 2 smaller than predicted based on archival data from the CSO test radio interferometer. It is postulated that part of the difference is attributable to surface-layer water vapor turbulence, which would be smaller at the elevation of the Keck telescopes than for the test antennas, similar to surface-layer effects seen in dry air seeing at Mauna Kea. The midfrequency power spectral amplitude better characterizes the residuals for a feedforward compensation system, and this value is found to be a factor of 65 smaller at K band for water vapor than for dry air; the difference compared to the ratio of the rms values is attributable to the lower effective wind speed of the water vapor turbulence, and thus lower control bandwidths are required for compensation than a simple scaling based on rms fluctuations would indicate. The water vapor coherence time is also shown to have modest correlations with both precipitable water vapor and the dry air coherence time, although the variability of the water vapor turbulence strength is larger than that of the dry air turbulence.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Colavita, MM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Mark.Colavita@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); W. M. Keck
Foundation
FX Thanks to Rachel Akeson and Oliver Lay for helpful comments, and to
Claude Felizardo for assistance with the data processing. Thanks also to
the referee for helpful suggestions. The Keck Interferometer is funded
by the National Aeronautics and Space Administration (NASA).
Observations presented 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 NASA. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. This work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
NR 31
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U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD JUN
PY 2010
VL 122
IS 892
BP 712
EP 721
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 600NK
UT WOS:000277993400008
ER
PT J
AU Becker-Reshef, I
Justice, C
Sullivan, M
Vermote, E
Tucker, C
Anyamba, A
Small, J
Pak, E
Masuoka, E
Schmaltz, J
Hansen, M
Pittman, K
Birkett, C
Williams, D
Reynolds, C
Doorn, B
AF Becker-Reshef, Inbal
Justice, Chris
Sullivan, Mark
Vermote, Eric
Tucker, Compton
Anyamba, Assaf
Small, Jen
Pak, Ed
Masuoka, Ed
Schmaltz, Jeff
Hansen, Matthew
Pittman, Kyle
Birkett, Charon
Williams, Derrick
Reynolds, Curt
Doorn, Bradley
TI Monitoring Global Croplands with Coarse Resolution Earth Observations:
The Global Agriculture Monitoring (GLAM) Project
SO REMOTE SENSING
LA English
DT Article
DE agriculture; monitoring; MODIS; croplands; GLAM
AB In recent years there has been a dramatic increase in the demand for timely, comprehensive global agricultural intelligence. Timely information on global crop production is indispensable for combating the growing stress on the world's crop production and for securing both short-term and long-term stable and reliable supply of food. Global agriculture monitoring systems are critical to providing this kind of intelligence and global earth observations are an essential component of an effective global agricultural monitoring system as they offer timely, objective, global information on croplands distribution, crop development and conditions as the growing season progresses. The Global Agriculture Monitoring Project (GLAM), a joint NASA, USDA, UMD and SDSU initiative, has built a global agricultural monitoring system that provides the USDA Foreign Agricultural Service (FAS) with timely, easily accessible, scientifically-validated remotely-sensed data and derived products as well as data analysis tools, for crop-condition monitoring and production assessment. This system is an integral component of the USDA's FAS Decision Support System (DSS) for agriculture. It has significantly improved the FAS crop analysts' ability to monitor crop conditions, and to quantitatively forecast crop yields through the provision of timely, high-quality global earth observations data in a format customized for FAS alongside a suite of data analysis tools. FAS crop analysts use these satellite data in a 'convergence of evidence' approach with meteorological data, field reports, crop models, attache reports and local reports. The USDA FAS is currently the only operational provider of timely, objective crop production forecasts at the global scale. These forecasts are routinely used by the other US Federal government agencies as well as by commodity trading companies, farmers, relief agencies and foreign governments. This paper discusses the operational components and new developments of the GLAM monitoring system as well as the future role of earth observations in global agricultural monitoring.
C1 [Becker-Reshef, Inbal; Justice, Chris; Sullivan, Mark; Vermote, Eric] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Tucker, Compton; Anyamba, Assaf; Small, Jen; Pak, Ed; Masuoka, Ed; Schmaltz, Jeff] NASA, Goddard Space & Flight Ctr, Greenbelt, MD 20771 USA.
[Hansen, Matthew; Pittman, Kyle] S Dakota State Univ, Geog Informat Sci Ctr Excellence, Brookings, SD 57007 USA.
[Birkett, Charon] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Williams, Derrick; Reynolds, Curt] Foreign Agr Serv, USDA, Washington, DC 20250 USA.
[Doorn, Bradley] NASA Head Quarters, Washington, DC 20546 USA.
RP Becker-Reshef, I (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
EM ireshef@hermes.geog.edu; justice@hermes.geog.umd.edu;
mbs@hermes.geog.umd.edu; eric@ltdri.org; Compton.j.tucker@nasa.gov;
Asaph.anyamba-1@nasa.gov; jennifer.l.small@nasa.gov;
Edwin.w.pak@nasa.gov; Edward.j.masuoka@nasa.gov; jeff.schmaltz@nasa.gov;
matthew.hansen@sdstate.edu; kyle.pittman@sdstate.edu; cmb@essic.umd.edu;
derrick.williams@fas.usda.gov; curt.reynolds@fas.usda.gov;
bradley.doorn@nasa.gov
RI Vermote, Eric/K-3733-2012
FU NASA; USDA Foreign Agricultural Service [NNS06AA03A]
FX The Global Agricultural Monitoring Project is made possible through
funding provided by the NASA Applied Science Program and the USDA
Foreign Agricultural Service, grant code NNS06AA03A.
NR 25
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PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JUN
PY 2010
VL 2
IS 6
BP 1589
EP 1609
DI 10.3390/rs2061589
PG 21
WC Remote Sensing
SC Remote Sensing
GA V24HN
UT WOS:000208401600011
ER
PT J
AU Richardson, IG
Cane, HV
AF Richardson, I. G.
Cane, H. V.
TI Near-Earth Interplanetary Coronal Mass Ejections During Solar Cycle 23
(1996-aEuro parts per thousand 2009): Catalog and Summary of Properties
SO SOLAR PHYSICS
LA English
DT Article
DE Coronal mass ejections; Interplanetary coronal mass ejections;
Interplanetary magnetic field; Magnetic clouds; Solar wind plasma
ID RIEGER-TYPE PERIODICITIES; FLIGHT-CENTER INSTRUMENTS; WIND HELIUM
ABUNDANCE; INTER-PLANETARY SHOCK; MAGNETIC CLOUDS; ENERGETIC PARTICLES;
CHARGE STATES; IONIZATION STATE; SOURCE LOCATION; SUNSPOT AREAS
AB In a previous study (Cane and Richardson, J. Geophys. Res. 108(A4), SSH6-1, 2003), we investigated the occurrence of interplanetary coronal mass ejections in the near-Earth solar wind during 1996 -aEuro parts per thousand 2002, corresponding to the increasing and maximum phases of solar cycle 23, and provided a "comprehensive" catalog of these events. In this paper, we present a revised and updated catalog of the a parts per thousand 300 near-Earth ICMEs in 1996 -aEuro parts per thousand 2009, encompassing the complete cycle 23, and summarize their basic properties and geomagnetic effects. In particular, solar wind composition and charge state observations are now considered when identifying the ICMEs. In general, these additional data confirm the earlier identifications based predominantly on other solar wind plasma and magnetic field parameters. However, the boundaries of ICME-like plasma based on charge state/composition data may deviate significantly from those based on conventional plasma/magnetic field parameters. Furthermore, the much studied "magnetic clouds", with flux-rope-like magnetic field configurations, may form just a substructure of the total ICME interval.
C1 [Richardson, I. G.; Cane, H. V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, I. G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, I. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cane, H. V.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov; hilary.cane@utas.edu.au
OI Richardson, Ian/0000-0002-3855-3634
FU NASA
FX We are indebted to all the experimenters who have produced and
generously made available the various data sets used to compile this
catalog. The LASCO CME catalog is generated and maintained at the
CDAWData Center by NASA and The Catholic University of America in
cooperation with the Naval Research Laboratory. SOHO is a project of
international cooperation between ESA and NASA. This work was funded by
a NASA Heliosphysics Guest Investigator award.
NR 103
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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 JUN
PY 2010
VL 264
IS 1
BP 189
EP 237
DI 10.1007/s11207-010-9568-6
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 610OM
UT WOS:000278742600013
ER
PT J
AU Krupp, N
Khurana, KK
Iess, L
Lainey, V
Cassidy, TA
Burger, M
Sotin, C
Neubauer, F
AF Krupp, N.
Khurana, K. K.
Iess, L.
Lainey, V.
Cassidy, T. A.
Burger, M.
Sotin, C.
Neubauer, F.
TI Environments in the Outer Solar System
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Planetary magnetospheres; Plasma transport; Jupiter; Saturn; Icy moons;
Magnetosphere moon interaction
ID LOW-ENERGY PLASMA; FLOW PAST IO; GALILEAN SATELLITES; MAGNETIC-FIELD;
INTERNAL STRUCTURE; JOVIAN MAGNETOSPHERE; GRAVITY-FIELD; NEPTUNE
MAGNETOSPHERE; ACCURATE EPHEMERIDES; URANIAN SATELLITES
AB The outer planets of our solar system Jupiter, Saturn, Uranus, and Neptune are fascinating objects on their own. Their intrinsic magnetic fields form magnetic environments (so called magnetospheres) in which charged and neutral particles and dust are produced, lost or being transported through the system. These magnetic environments of the gas giants can be envisaged as huge plasma laboratories in space in which electromagnetic waves, current systems, particle transport mechanisms, acceleration processes and other phenomena act and interact with the large number of moons in orbit around those massive planets.
In general it is necessary to describe and study the global environments (magnetospheres) of the gas giants, its global configuration with its large-scale transport processes; and, in combination, to study the local environments of the moons as well, e.g. the interaction processes between the magnetospheric plasma and the exosphere/atmosphere/magnetosphere of the moon acting on time scales of seconds to days. These local exchange processes include also the gravity, shape, rotation, astrometric observations and orbital parameters of the icy moons in those huge systems.
It is the purpose of this chapter of the book to describe the variety of the magnetic environments of the outer planets in a broad overview, globally and locally, and to show that those exchange processes can dramatically influence the surfaces and exospheres/atmospheres of the moons and they can also be used as a tool to study the overall physics of systems as a whole.
C1 [Krupp, N.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Khurana, K. K.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA.
[Iess, L.] Univ Roma La Sapienza, Dipartimento Ingn Aerosp & Astronaut, Rome, Italy.
[Lainey, V.] IMCCE Observ Paris, Paris, France.
[Cassidy, T. A.] Univ Virginia, Charlottesville, VA USA.
[Burger, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Neubauer, F.] Univ Cologne, Cologne, Germany.
RP Krupp, N (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
EM krupp@mps.mpg.de
RI IESS, Luciano/F-4902-2011; Burger, Matthew/C-1310-2011
OI IESS, Luciano/0000-0002-6230-5825;
FU EC [001637]; German Space Agency DLR [50OH0801, 50OH0802]; Max Planck
Society; NASA
FX This work was financed through the EC contract No. 001637 (RICA)
EURO-PLANET. Work at the Max-Planck-Institut fur Sonnensystemforschung
has been supported by the German Space Agency DLR through the contracts
50OH0801 and 50OH0802 and by the Max Planck Society. Work in the US has
been supported by NASA. V.L. thanks J.-E. Arlot and A. Vienne for
fruitful discussions.
NR 136
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U2 12
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 JUN
PY 2010
VL 153
IS 1-4
BP 11
EP 59
DI 10.1007/s11214-010-9653-z
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200003
ER
PT J
AU Prockter, LM
Lopes, RMC
Giese, B
Jaumann, R
Lorenz, RD
Pappalardo, RT
Patterson, GW
Thomas, PC
Turtle, EP
Wagner, RJ
AF Prockter, Louise M.
Lopes, Rosaly M. C.
Giese, Bernd
Jaumann, Ralf
Lorenz, Ralph D.
Pappalardo, Robert T.
Patterson, Gerald W.
Thomas, Peter C.
Turtle, Elizabeth P.
Wagner, Roland J.
TI Characteristics of Icy Surfaces
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Icy satellites; Europa; Ganymede; Titan; Enceladus; Cryovolcanism
ID INFRARED MAPPING SPECTROMETER; CASSINI IMAGING SCIENCE; GALILEO NOMINAL
MISSION; SMALL INNER SATELLITES; SOUTH-POLAR FRACTURES; CONAMARA CHAOS
REGION; TITANS SURFACE; GROOVED TERRAIN; WATER-ICE; PLANETARY SCIENCE
AB The surfaces of the Solar System's icy satellites show an extraordinary variety of morphological features, which bear witness to exchange processes between the surface and subsurface. In this paper we review the characteristics of surface features on the moons of Jupiter, Saturn, Uranus and Neptune. Using data from spacecraft missions, we discuss the detailed morphology, size, and topography of cryovolcanic, tectonic, aeolian, fluvial, and impact features of both large moons and smaller satellites.
C1 [Prockter, Louise M.; Lorenz, Ralph D.; Patterson, Gerald W.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Lopes, Rosaly M. C.; Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Giese, Bernd; Jaumann, Ralf; Wagner, Roland J.] Inst Planetary Res, German Aerosp Ctr DLR, D-12489 Berlin, Germany.
[Thomas, Peter C.] Cornell Univ, Ithaca, NY 14853 USA.
RP Prockter, LM (reprint author), Johns Hopkins Univ, Appl Phys Lab, MP3-E169,11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Louise.Prockter@jhuapl.edu
RI Turtle, Elizabeth/K-8673-2012; Patterson, Gerald/E-7699-2015; Lorenz,
Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016
OI Turtle, Elizabeth/0000-0003-1423-5751; Lorenz,
Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167
FU National Aeronautics and Space Administration
FX We thank two anonymous reviewers for their helpful comments, and Olivier
Grasset for his tireless efforts in putting together this volume. The
portions of this work performed by RTP and RMCL were carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 283
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U2 25
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 63
EP 111
DI 10.1007/s11214-010-9649-8
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200004
ER
PT J
AU Dalton, JB
Cruikshank, DP
Stephan, K
McCord, TB
Coustenis, A
Carlson, RW
Coradini, A
AF Dalton, J. B.
Cruikshank, D. P.
Stephan, K.
McCord, T. B.
Coustenis, A.
Carlson, R. W.
Coradini, A.
TI Chemical Composition of Icy Satellite Surfaces
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Composition; Icy satellites; Infrared spectroscopy
ID INFRARED MAPPING SPECTROMETER; HUBBLE-SPACE-TELESCOPE; HUYGENS LANDING
SITE; EXTREME ULTRAVIOLET OBSERVATIONS; PHOTOCHEMICAL FLOW REACTOR;
TITANS UPPER-ATMOSPHERE; HYDRATED SALT MINERALS; KUIPER-BELT OBJECTS;
JUPITERS MOON IO; 5 MU-M
AB Much of our knowledge of planetary surface composition is derived from remote sensing over the ultraviolet through infrared wavelength ranges. Telescopic observations and, in the past few decades, spacecraft mission observations have led to the discovery of many surface materials, from rock-forming minerals to water ice to exotic volatiles and organic compounds. Identifying surface materials and mapping their distributions allows us to constrain interior processes such as cryovolcanism and aqueous geochemistry.
The recent progress in understanding of icy satellite surface composition has been aided by the evolving capabilities of spacecraft missions, advances in detector technology, and laboratory studies of candidate surface compounds. Pioneers 10 and 11, Voyagers I and II, Galileo, Cassini and the New Horizons mission have all made significant contributions. Dalton (Space Sci. Rev., 2010, this issue) summarizes the major constituents found or inferred to exist on the surfaces of the icy satellites (cf. Table 1 from Dalton, Space Sci. Rev., 2010, this issue), and the spectral coverage and resolution of many of the spacecraft instruments that have revolutionized our understanding (cf. Table 2 from Dalton, Space Sci. Rev., 2010, this issue). While much has been gained from these missions, telescopic observations also continue to provide important constraints on surface compositions, especially for those bodies that have not yet been visited by spacecraft, such as Kuiper Belt Objects (KBOs), trans-Neptunian Objects (TNOs), Centaurs, the classical planet Pluto and its moon, Charon.
In this chapter, we will discuss the major satellites of the outer solar system, the materials believed to make up their surfaces, and the history of some of these discoveries. Formation scenarios and subsequent evolution will be described, with particular attention to the processes that drive surface chemistry and exchange with interiors. Major similarities and differences between the satellites are discussed, with an eye toward elucidating processes operating throughout the outer solar system. Finally we discuss the outermost satellites and other bodies, and summarize knowledge of their composition. Much of this review is likely to change in the near future with ongoing and planned outer planet missions, adding to the sense of excitement and discovery associated with our exploration of our planetary neighborhood.
C1 [Dalton, J. B.; Carlson, R. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cruikshank, D. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stephan, K.] German Aerosp Ctr DLR, D-12489 Berlin, Germany.
[McCord, T. B.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Coustenis, A.] Observ Paris, LESIA, F-92195 Meudon, France.
[Coradini, A.] IFSI, I-00133 Rome, Italy.
RP Dalton, JB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dalton@jpl.nasa.gov
FU National Aeronautics and Space Administration; NASA; European Space
Agency (ESA); German Aerospace Center (DLR); Italian Istituto di Fisica
della Spazio Interplanetario (IFSI)
FX A portion of 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. The authors
acknowledge the support of the NASA Outer Planets and Cassini Data
Analysis programs, the European Space Agency (ESA), the German Aerospace
Center (DLR), and the Italian Istituto di Fisica della Spazio
Interplanetario (IFSI).
NR 342
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U2 49
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 JUN
PY 2010
VL 153
IS 1-4
BP 113
EP 154
DI 10.1007/s11214-010-9665-8
PG 42
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200005
ER
PT J
AU Coustenis, A
Tokano, T
Burger, MH
Cassidy, TA
Lopes, RM
Lorenz, RD
Retherford, KD
Schubert, G
AF Coustenis, A.
Tokano, T.
Burger, M. H.
Cassidy, T. A.
Lopes, R. M.
Lorenz, R. D.
Retherford, K. D.
Schubert, G.
TI Atmospheric/Exospheric Characteristics of Icy Satellites
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Atmospheres; Exospheres; Icy satellites; Titan; Io; Enceladus; Europa
ID HUBBLE-SPACE-TELESCOPE; GALILEO ULTRAVIOLET SPECTROMETER; COMPOSITE
INFRARED SPECTROMETER; VOLCANICALLY DRIVEN ATMOSPHERE; RADIO OCCULTATION
MEASUREMENTS; TITANS SOUTH-POLE; IOS PELE PLUME; ADAPTIVE OPTICS; SO2
ATMOSPHERE; CASSINI RADAR
AB The atmospheres/exospheres of icy satellites greatly vary from one to the next in terms of density, composition, structure or steadiness. Titan is the only icy satellite with a dense atmosphere comparable in many ways to that of the Earth's atmosphere. Titan's atmosphere prevents the surface from direct interaction with the plasma environment, but gives rise to Earth-like exchanges of energy, matter and momentum. The atmospheres of other satellites are tenuous. Enceladus' atmosphere manifests itself in a large water vapor plume emanating from surface cracks near the south pole. Io's SO2 atmosphere originates from volcanoes. Europa's tenuous O-2 atmosphere is produced by intense radiation bombardment. This chapter reviews the characteristics of the atmospheres of Titan, Enceladus, Io and Europa based on observations.
C1 [Coustenis, A.] Observ Paris, LESIA, F-92195 Meudon, France.
[Tokano, T.] Univ Cologne, Inst Geophys & Meteorol, D-5000 Cologne, Germany.
[Burger, M. H.] Univ Maryland, Greenbelt, MD 20771 USA.
[Burger, M. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cassidy, T. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Lopes, R. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Retherford, K. D.] SW Res Inst, San Antonio, TX USA.
[Schubert, G.] Univ Calif Los Angeles, Los Angeles, CA USA.
RP Coustenis, A (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM athena.coustenis@obspm.fr
RI Burger, Matthew/C-1310-2011; Lorenz, Ralph/B-8759-2016; Lopes,
Rosaly/D-1608-2016
OI Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167
NR 194
TC 4
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U2 12
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 JUN
PY 2010
VL 153
IS 1-4
BP 155
EP 184
DI 10.1007/s11214-009-9615-5
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200006
ER
PT J
AU Fortes, AD
Choukroun, M
AF Fortes, A. Dominic
Choukroun, Mathieu
TI Phase Behaviour of Ices and Hydrates
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Water ice; Methane clathrate; Ammonia; Methanol; Sulfuric acid;
Sulfates; Polymorphism; Phase relations
ID NEUTRON POWDER DIFFRACTION; AMMONIA-WATER SYSTEM; HIGH-PRESSURE PHASE;
OUTER SOLAR-SYSTEM; EQUATION-OF-STATE; METHANE CLATHRATE HYDRATE;
SULFURIC-ACID-SOLUTIONS; X-RAY-DIFFRACTION; CRYSTAL-STRUCTURE; ICY
SATELLITES
AB The primary volatile 'rock-forming' minerals in the icy satellites of the outer solar system include water-ice and various hydrated crystals of methane and ammonia. The rich polymorphism of these substances as a function of pressure and temperature are described in this chapter. This polymorphism has a fundamental influence on the exchange of mass and energy between the core and the surface of icy satellites. We describe the current state-of-the-art in our understanding of the high pressure phase behaviour and the measurements of thermoelastic and transport properties of these substances. In addition we describe the structures and properties of hydrated phases of methanol, sulfuric acid, and various sulfate salts.
C1 [Fortes, A. Dominic] UCL Birkbeck, Ctr Planetary Sci, London WC1E 6BT, England.
[Choukroun, Mathieu] NASA, Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA.
RP Fortes, AD (reprint author), UCL Birkbeck, Ctr Planetary Sci, Gower St, London WC1E 6BT, England.
EM andrew.fortes@ucl.ac.uk; mathieu.choukroun@jpl.nasa.gov
RI Fortes, Andrew/C-1349-2011; Choukroun, Mathieu/F-3146-2017
OI Fortes, Andrew/0000-0001-5907-2285; Choukroun,
Mathieu/0000-0001-7447-9139
FU UK Science and Technology Facilities Council (STFC) [PP/E006515/1];
NASA; Oak Ridge Associated Universities
FX ADF is supported by an Advanced Fellowship from the UK Science and
Technology Facilities Council (STFC), grant number PP/E006515/1. MC is
supported by a NASA Postdoctoral Fellowship, administered by Oak Ridge
Associated Universities. Part of this work has been conducted at the Jet
Propulsion Laboratory, California Institute of Technology. Copyright
2009. All rights reserved. Government sponsorship acknowledged.
NR 254
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SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 185
EP 218
DI 10.1007/s11214-010-9633-3
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200007
ER
PT J
AU Dalton, JB
AF Dalton, J. B.
TI Spectroscopy of Icy Moon Surface Materials
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Ice; Infrared spectroscopy; Remote sensing; Planetary science
ID GALILEO PHOTOPOLARIMETER-RADIOMETER; ULTRAVIOLET SPECTROMETER
EXPERIMENT; NEAR-INFRARED SPECTROSCOPY; OUTER SOLAR-SYSTEM; POLYCYCLIC
AROMATIC-HYDROCARBONS; COMPLEX REFRACTIVE-INDEXES; CM(-1)
OPTICAL-CONSTANTS; SOLID CARBON MONOXIDE; 5 MU-M; WATER-ICE
AB Remote sensing of icy objects in the outer solar system relies upon availability of appropriate laboratory measurements. Surface deposits of specific substances often provide our most direct route to understanding interior composition, thereby informing theories of endogenic surface modification, exogenic surface processing and processes involving exchange of material with the interiors. Visible to near-infrared reflectance spectra of properly prepared compounds are required to enable retrieval of surface abundances through linear and nonlinear mixture analysis applied to spacecraft observations of icy bodies. This chapter describes the techniques, conditions and approaches necessary to provide reference spectra of use to theoretical models of icy satellite surface compositions, and summarizes the current state of knowledge represented in the published literature.
C1 CALTECH, Jet Prop Lab, Planetary Ices Grp, Pasadena, CA 91109 USA.
RP Dalton, JB (reprint author), CALTECH, Jet Prop Lab, Planetary Ices Grp, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dalton@jpl.nasa.gov
FU NASA; Jet Propulsion Laboratory
FX The author wishes to express his gratitude to Barbara Amago, Robert
Powers and Marion Hernandez of the Jet Propulsion Laboratory Technical
Library for their assistance with this article. Corey Jamieson, Jake
Cooper and Saveelah Talib contributed to Table 3. This work was
supported by the NASA Outer Planets Research Program and the Jet
Propulsion Laboratory Research and Technology Development Program.
NR 258
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 219
EP 247
DI 10.1007/s11214-010-9658-7
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200008
ER
PT J
AU Cassidy, T
Coll, P
Raulin, F
Carlson, RW
Johnson, RE
Loeffler, MJ
Hand, KP
Baragiola, RA
AF Cassidy, T.
Coll, P.
Raulin, F.
Carlson, R. W.
Johnson, R. E.
Loeffler, M. J.
Hand, K. P.
Baragiola, R. A.
TI Radiolysis and Photolysis of Icy Satellite Surfaces: Experiments and
Theory
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Radiolysis; Photolysis; Sputtering; Tholins; Ices
ID SOLAR-SYSTEM SURFACES; WATER-ICE; ION IRRADIATION; SULFURIC-ACID;
GALILEAN SATELLITES; OPTICAL-CONSTANTS; TITANS THOLINS; X-RAY; MU-M;
EUROPA
AB The transport and exchange of material between bodies in the outer solar system is often facilitated by their exposure to ionizing radiation. With this in mind we review the effects of energetic ions, electrons and UV photons on materials present in the outer solar system. We consider radiolysis, photolysis, and sputtering of low temperature solids. Radiolysis and photolysis are the chemistry that follows the bond breaking and ionization produced by incident radiation, producing, e.g., O-2 and H-2 from irradiated H2O ice. Sputtering is the ejection of molecules by incident radiation. Both processes are particularly effective on ices in the outer solar system. Materials reviewed include H2O ice, sulfur-containing compounds (such as SO2 and S-8), carbon-containing compounds (such as CH4), nitrogen-containing compounds (such as NH3 and N-2), and mixtures of those compounds. We also review the effects of ionizing radiation on a mixture of N-2 and CH4 gases, as appropriate to Titan's upper atmosphere, where radiolysis and photolysis produce complex organic compounds (tholins).
C1 [Cassidy, T.; Carlson, R. W.; Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cassidy, T.; Johnson, R. E.] Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA.
[Coll, P.] Univ Paris 07, Lab Interuniv Syst Atmospher, Creteil, France.
[Raulin, F.] Univ Paris 7 & Paris 12, Lab Interuniv Syst Atmospher, UMR 7583, Creteil, France.
[Johnson, R. E.] New York Univ, Dept Phys, New York, NY 10003 USA.
[Loeffler, M. J.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
[Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
RP Cassidy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tac2z@virginia.edu
RI Loeffler, Mark/C-9477-2012
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 299
EP 315
DI 10.1007/s11214-009-9625-3
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200011
ER
PT J
AU Hussmann, H
Choblet, G
Lainey, V
Matson, DL
Sotin, C
Tobie, G
Van Hoolst, T
AF Hussmann, Hauke
Choblet, Gael
Lainey, Valery
Matson, Dennis L.
Sotin, Christophe
Tobie, Gabriel
Van Hoolst, Tim
TI Implications of Rotation, Orbital States, Energy Sources, and Heat
Transport for Internal Processes in Icy Satellites
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Satellites; Energy sources; Rotation; Tides; Orbital dynamics; Heat
transfer
ID JUPITERS GALILEAN SATELLITES; PRANDTL NUMBER FLUID; GEYSER-LIKE PLUMES;
TIDAL DISSIPATION; SOLAR-SYSTEM; THERMAL-CONVECTION; DEPENDENT
VISCOSITY; INTERIOR STRUCTURE; VOLCANIC ACTIVITY; SOUTH-POLE
AB Internal processes in icy satellites, e.g. the exchange of material from the subsurface to the surface or processes leading to volcanism and resurfacing events, are a consequence of the amount of energy available in the satellites' interiors. The latter is mainly determined shortly after accretion by the amount of radioactive isotopes incorporated in the silicates during the accretion process. However, for satellites-as opposed to single objects-important contributions to the energy budget on long time-scales can come from the interaction with other satellites (forcing of eccentricities of satellites in resonance) and consequently from the tidal interaction with the primary planet. Tidal evolution involves both changes of the rotation state-usually leading to the 1:1 spin orbit coupling-and long-term variations of the satellite orbits. Both processes are dissipative and thus connected with heat production in the interior. The way heat is transported from the interior to the surface (convection, conduction, (cryo-) volcanism) is a second main aspect that determines how internal processes in satellites work. In this chapter we will discuss the physics of heat production and heat transport as well as the rotational and orbital states of satellites. The relevance of the different heat sources for the moons in the outer solar system are compared and discussed.
C1 [Hussmann, Hauke] DLR Inst Planetary Res, D-12489 Berlin, Germany.
[Choblet, Gael; Tobie, Gabriel] Univ Nantes, Lab Planetol & Geodynam, F-44322 Nantes, France.
[Lainey, Valery] Observ Paris 77, IMCCE, F-75014 Paris, France.
[Matson, Dennis L.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Van Hoolst, Tim] Royal Observ Belgium, B-1180 Brussels, Belgium.
RP Hussmann, H (reprint author), DLR Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM hauke.hussmann@dlr.de
FU NASA; Helmholtz Association
FX Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. Part of
this work has been supported by the Helmholtz Association through the
alliance 'Planetary Evolution and Life'.
NR 117
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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 JUN
PY 2010
VL 153
IS 1-4
BP 317
EP 348
DI 10.1007/s11214-010-9636-0
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200012
ER
PT J
AU Burger, MH
Wagner, R
Jaumann, R
Cassidy, TA
AF Burger, Matthew H.
Wagner, Roland
Jaumann, Ralf
Cassidy, Timothy A.
TI Effects of the External Environment on Icy Satellites
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Planetary science; Atmospheres; Magnetospheres; Outer solar system;
Satellites; Solar system evolution; Surfaces; Impact histories
ID IO PLASMA TORUS; CASSINI UVIS OBSERVATIONS; JUPITER-FAMILY COMETS;
ELECTRON-IMPACT IONIZATION; OUTER SOLAR-SYSTEM; CROSS-SECTIONS; IMAGING
SCIENCE; GALILEAN SATELLITES; COLLISIONAL EVOLUTION; AZIMUTHAL
VARIABILITY
AB In order to understand the evolution of planetary satellite surfaces and atmospheres it is important to understand their external environments. In this paper we look at the interactions between plasma in planetary magnetospheres and satellite atmospheres responsible for the production and loss of atmospheric mass. We focus on the processes which take place in the tenuous atmospheres of the Galilean satellites and in the Enceladus water plume. We also review the impact histories of satellites in the outer solar system, and compare the record of impacts in the inner and outer solar system.
C1 [Burger, Matthew H.] Univ Maryland, Greenbelt, MD USA.
[Burger, Matthew H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wagner, Roland; Jaumann, Ralf] DLR, Berlin, Germany.
[Cassidy, Timothy A.] Univ Virginia, Charlottesville, VA USA.
RP Burger, MH (reprint author), Univ Maryland, Greenbelt, MD USA.
EM Matthew.H.Burger@nasa.gov
RI Burger, Matthew/C-1310-2011
NR 123
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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 JUN
PY 2010
VL 153
IS 1-4
BP 349
EP 374
DI 10.1007/s11214-010-9645-z
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200013
ER
PT J
AU Tobie, G
Giese, B
Hurford, TA
Lopes, RM
Nimmo, F
Postberg, F
Retherford, KD
Schmidt, J
Spencer, JR
Tokano, T
Turtle, EP
AF Tobie, G.
Giese, B.
Hurford, T. A.
Lopes, R. M.
Nimmo, F.
Postberg, F.
Retherford, K. D.
Schmidt, J.
Spencer, J. R.
Tokano, T.
Turtle, E. P.
TI Surface, Subsurface and Atmosphere Exchanges on the Satellites of the
Outer Solar System
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Subsurface; Surface; Atmosphere; Icy moons
ID INFRARED MAPPING SPECTROMETER; CASSINI RADAR OBSERVATIONS; SOUTH-POLAR
FRACTURES; LARGE IMPACT FEATURES; ICE SHELL THICKNESS; TITANS SURFACE;
ENCELADUS PLUME; HUYGENS PROBE; HEAT-FLUX; GALILEAN SATELLITES
AB The surface morphology of icy moons is affected by several processes implicating exchanges between their subsurfaces and atmospheres (if any). The possible exchange of material between the subsurface and the surface is mainly determined by the mechanical properties of the lithosphere, which isolates the deep, warm and ductile ice material from the cold surface conditions. Exchanges through this layer occur only if it is sufficiently thin and/or if it is fractured owing to tectonic stresses, melt intrusion or impact cratering. If such conditions are met, cryomagma can be released, erupting fresh volatile-rich materials onto the surface. For a very few icy moons (Titan, Triton, Enceladus), the emission of gas associated with cryovolcanic activity is sufficiently large to generate an atmosphere, either long-lived or transient. For those moons, atmosphere-driven processes such as cryovolcanic plume deposition, phase transitions of condensable materials and wind interactions continuously re-shape their surfaces, and are able to transport cryovolcanically generated materials on a global scale. In this chapter, we discuss the physics of these different exchange processes and how they affect the evolution of the satellites' surfaces.
C1 [Tobie, G.] Univ Nantes Atlantique, Lab Planetol & Geodynam Nantes, F-44322 Nantes 03, France.
[Tobie, G.] CNRS, UMR 6112, F-44322 Nantes 03, France.
[Giese, B.] Inst Planetary Res, German Aerosp Ctr, D-12489 Berlin, Germany.
[Hurford, T. A.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Lopes, R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Postberg, F.] Heidelberg Univ, Inst Earth Sci, D-69120 Heidelberg, Germany.
[Postberg, F.] Max Planck Inst Kernphys MPI Nucl Phys, D-69117 Heidelberg, Germany.
[Retherford, K. D.] SW Res Inst, San Antonio, TX 78228 USA.
[Schmidt, J.] Univ Potsdam, D-14469 Potsdam, Germany.
[Spencer, J. R.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Tokano, T.] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany.
[Turtle, E. P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Tobie, G (reprint author), Univ Nantes Atlantique, Lab Planetol & Geodynam Nantes, F-44322 Nantes 03, France.
EM gabriel.tobie@univ-nantes.fr
RI Hurford, Terry/F-2625-2012; Turtle, Elizabeth/K-8673-2012; Lopes,
Rosaly/D-1608-2016
OI Turtle, Elizabeth/0000-0003-1423-5751; Lopes, Rosaly/0000-0002-7928-3167
FU INSU; NASA
FX We thank L. Soderblom for helpful suggestions and corrections. Supports
from INSU's Programme National de Planetologie, NASA's Planetary Geology
and Geophysics and Outer Planets Research programmes are gratefully
acknowledged.
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PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 375
EP 410
DI 10.1007/s11214-010-9641-3
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200014
ER
PT J
AU Schubert, G
Hussmann, H
Lainey, V
Matson, DL
McKinnon, WB
Sohl, F
Sotin, C
Tobie, G
Turrini, D
Van Hoolst, T
AF Schubert, G.
Hussmann, H.
Lainey, V.
Matson, D. L.
McKinnon, W. B.
Sohl, F.
Sotin, C.
Tobie, G.
Turrini, D.
Van Hoolst, T.
TI Evolution of Icy Satellites
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Outer planet moons; Io; Europa; Enceladus; Dione; Titan; Iapetus; Rhea;
Tethys; Phoebe; Pluto; Charon; Satellite evolution
ID KUIPER-BELT OBJECTS; NEAR-INFRARED SPECTROSCOPY; GIANT IMPACT ORIGIN;
OUTER SOLAR-SYSTEM; IOS HEAT-FLOW; THERMAL EVOLUTION; IRREGULAR
SATELLITES; GALILEAN SATELLITES; TIDAL DISSIPATION; VISCOELASTIC MODELS
AB Evolutionary scenarios for the major satellites of Jupiter, Saturn, Neptune, and Pluto-Charon are discussed. In the Jovian system the challenge is to understand how the present Laplace resonance of Io, Europa, and Ganymede was established and to determine whether the heat being radiated by Io is in balance with the present tidal dissipation in the moon. In the Saturnian system, Enceladus and Titan are the centers of attention. Tidal heating is the likely source of activity at the south pole of Enceladus, although the details of how the heating occurs are not understood. An evolutionary scenario based on accretion and internal differentiation is presented for Titan, whose present substantial orbital eccentricity is not associated with any dynamical resonance. The source and maintenance of methane in Titan's present atmosphere remain uncertain. Though most attention on the Saturnian moons focuses on Titan and Enceladus, the mid-size satellites Iapetus, Rhea, Tethys, and the irregular satellite Phoebe also draw our interest. An evolutionary scenario for Iapetus is presented in which spin down from an early rapidly rotating state is called upon to explain the satellite's present oblate shape. The prominent equatorial ridge on Iapetus is unexplained by the spin down scenario. A buckling instability provides another possible explanation for the oblateness and equatorial ridge of Iapetus. Rhea is the only medium-size Saturnian satellite for which there are gravity data at present. The interpretation of these data are uncertain, however, since it is not known if Rhea is in hydrostatic equilibrium. Pluto and Charon are representative of the icy dwarf planets of the Kuiper belt. Did they differentiate as they evolved, and do either of them have a subsurface liquid water ocean? New Horizons might provide some answers when it arrives at these bodies.
C1 [Schubert, G.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Schubert, G.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Hussmann, H.; Sohl, F.] Inst Planetary Res, German Aerosp Ctr DLR, D-12489 Berlin, Germany.
[Lainey, V.] CNRS, IMCCE Observ Paris, UMR 8028, F-75014 Paris, France.
[Matson, D. L.] JPL 183 335, Pasadena, CA 91109 USA.
[McKinnon, W. B.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[McKinnon, W. B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tobie, G.] Univ Nantes, Nantes, France.
[Turrini, D.] INAF IFSI, I-00133 Rome, Italy.
[Van Hoolst, T.] Royal Observ Belgium, B-1180 Brussels, Belgium.
RP Schubert, G (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
EM schubert@ucla.edu; Hauke.Hussmann@dlr.de; Valery.Lainey@imcce.fr;
dennis.l.matson@jpl.nasa.gov; mckinnon@wustl.edu; Frank.Sohl@dlr.de;
christophe.sotin@jpl.nasa.gov; gabriel.tobie@univ-nantes.fr;
diego.turrini@ifsi-roma.inaf.it; tim.vanhoolst@oma.be
OI Turrini, Diego/0000-0002-1923-7740
FU NASA [NNG06GG70G]; New Horizons project
FX GS acknowledges support from the NASA Outer Planets Research and
Planetary Geology and Geophysics (NASA NNG06GG70G) programs. WBM thanks
the New Horizons project for support and S. A. Stern for comments.
NR 158
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U1 4
U2 37
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 447
EP 484
DI 10.1007/s11214-010-9635-1
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200017
ER
PT J
AU Sohl, F
Choukroun, M
Kargel, J
Kimura, J
Pappalardo, R
Vance, S
Zolotov, M
AF Sohl, Frank
Choukroun, Mathieu
Kargel, Jeffrey
Kimura, Jun
Pappalardo, Robert
Vance, Steve
Zolotov, Mikhail
TI Subsurface Water Oceans on Icy Satellites: Chemical Composition and
Exchange Processes
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Outer solar system; Water oceans; Oceanic composition; Chemical
evolution; Organic compounds; High-pressure ices; Clathrate hydrates;
Hydrothermal activity; Porous rock; Serpentinization; Europa; Ganymede;
Callisto; Titan; Enceladus
ID HYDRATED SALT MINERALS; INTERNAL STRUCTURE; GALILEAN SATELLITES;
HIGH-PRESSURES; NONSYNCHRONOUS ROTATION; HYDROTHERMAL SYSTEMS; CLATHRATE
FORMATION; INTERIOR STRUCTURE; TECTONIC PROCESSES; TIDAL DISSIPATION
AB The state of knowledge about the structure and composition of icy satellite interiors has been significantly extended by combining direct measurements from spacecraft, laboratory experiments, and theoretical modeling. The existence of potentially habitable liquid water reservoirs on icy satellites is dependent on the radiogenic heating of the rock component, additional contributions such as the dissipation of tidal energy, the efficiency of heat transfer to the surface, and the presence of substances that deplete the freezing point of liquid water. This review summarizes the chemical evolution of subsurface liquid water oceans, taking into account a number of chemical processes occuring in aqueous environments and partly related to material exchange with the deep interior. Of interest are processes occuring at the transitions from the liquid water layer to the ice layers above and below, involving the possible formation of clathrate hydrates and high-pressure ices on large icy satellites. In contrast, water-rock exchange is important for the chemical evolution of the liquid water layer if the latter is in contact with ocean floor rock on small satellites. The composition of oceanic floor deposits depends on ambient physical conditions and ocean chemistry, and their evolutions through time. In turn, physical properties of the ocean floor affect the circulation of oceanic water and related thermal effects due to tidally-induced porous flow and aqueous alteration of ocean floor rock.
C1 [Sohl, Frank] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Choukroun, Mathieu; Pappalardo, Robert; Vance, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Kargel, Jeffrey] Univ Arizona, Dept Hydrol, Tucson, AZ 85721 USA.
[Kimura, Jun] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Zolotov, Mikhail] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Sohl, F (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM frank.sohl@dlr.de; mathieu.choukroun@jpl.nasa.gov;
kargel@hwr.arizona.edu; junkim@ep.sci.hokudai.ac.jp;
robert.pappalardo@jpl.nasa.gov; svance@jpl.nasa.gov; zolotov@asu.edu
RI Kimura, Jun/D-6050-2013; Choukroun, Mathieu/F-3146-2017
OI Kimura, Jun/0000-0002-5825-0454; Choukroun, Mathieu/0000-0001-7447-9139
FU Helmholtz Association; National Aeronautics and Space Administration;
NASA; Caltech Postdoctoral Program
FX The authors are grateful to the organizers of the
EuroPlanet-ISSIWorkshop Exchange Processes on Icy Satellites, held
November 2008 in the inspiring environment of the International Space
Science Institute, Bern, Switzerland; two anonymous reviewers for their
constructive comments; and O. Grasset for the manuscript handling. We
would like to thank G. Tobie for providing the clathrate hydrates
densities calculations. This research has been supported by the
Helmholtz Association through the research alliance Planetary Evolution
and Life. A portion of this work was supported by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Doctors Choukroun,
Pappalardo and Vance acknowledge support from the NASA Astrobiology
Institute's Astrobiology of Icy Worlds program at the Jet Propulsion
Laboratory. Doctors Choukroun and Vance acknowledge support from the
NASA Postdoctoral Program administered by Oak Ridge Associated
Universities. S. Vance acknowledges support from the Caltech
Postdoctoral Program. F. Sohl acknowledges discussions with H. Hussmann,
V. Stamenkovic, and F. W. Wagner.
NR 134
TC 32
Z9 32
U1 8
U2 55
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD JUN
PY 2010
VL 153
IS 1-4
BP 485
EP 510
DI 10.1007/s11214-010-9646-y
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200018
ER
PT J
AU Raulin, F
Hand, KP
Mckay, CP
Viso, M
AF Raulin, Francois
Hand, Kevin P.
Mckay, Christopher P.
Viso, Michel
TI Exobiology and Planetary Protection of icy moons
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Exobiology; Prebiotic chemistry; Extraterrestrial life; Europa's ocean;
Enceladus liquid water reservoir; Habitability; Planetary protection
ID NEUTRAL MASS-SPECTROMETER; ENERGY-REQUIREMENTS; HYDROTHERMAL SYSTEMS;
HYPOTHESIZED OCEAN; INTERNAL STRUCTURE; HYDROGEN-PEROXIDE; TITANS
ATMOSPHERE; SURFACE ORGANICS; MICROBIAL LIFE; METHANE CYCLE
AB The outer solar system is an important area of investigation for exobiology, the study of life in the universe. Several moons of the outer planets involve processes and structures comparable to those thought to have played an important role in the emergence of life on Earth, such as the formation and exchange of organic materials between different reservoirs. The study of these prebiotic processes on, and in, outer solar system moons is a key goal for exobiology, together with the question of habitability and the search for evidence of past or even present life. This chapter reviews the aspects of prebiotic chemistry and potential presence of life on Europa, Enceladus and Titan, based on the most recent data obtained from space missions as well as theoretical and experimental laboratory models. The habitability of these extraterrestrial environments, which are likely to include large reservoirs of liquid water in their internal structure, is discussed as well as the particular case of Titan's hydrocarbon lakes. The question of planetary protection, especially in the case of Europa, is also presented.
C1 [Raulin, Francois] Univ Paris 7 & Paris 12, Creteil, France.
[Raulin, Francois] LISA CNRS, Creteil, France.
[Hand, Kevin P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Viso, Michel] CNES DSP EU, Paris, France.
RP Raulin, F (reprint author), Univ Paris 7 & Paris 12, Creteil, France.
EM Francois.Raulin@lisa.univ-paris12.fr; khand@jpl.nasa.gov;
chris.mckay@nasa.gov; michel.viso@cnes.fr
NR 106
TC 8
Z9 8
U1 3
U2 34
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 JUN
PY 2010
VL 153
IS 1-4
BP 511
EP 535
DI 10.1007/s11214-009-9610-x
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 657AA
UT WOS:000282381200019
ER
PT J
AU Lazarus, SM
Splitt, ME
Lueken, MD
Ramachandran, R
Li, XA
Movva, S
Graves, SJ
Zavodsky, BT
AF Lazarus, Steven M.
Splitt, Michael E.
Lueken, Michael D.
Ramachandran, Rahul
Li, Xiang
Movva, Sunil
Graves, Sara J.
Zavodsky, Bradley T.
TI Evaluation of Data Reduction Algorithms for Real-Time Analysis
SO WEATHER AND FORECASTING
LA English
DT Article
ID MEASURING INFORMATION-CONTENT; NUMERICAL WEATHER PREDICTION; DATA
ASSIMILATION; ATMOSPHERIC-TEMPERATURE; REMOTE MEASUREMENTS; OBJECTIVE
ANALYSIS; RECURSIVE FILTER; ANALYSIS SYSTEM; SATELLITE; DENSITY
AB Data reduction tools are developed and evaluated using a data analysis framework. Simple (nonadaptive) and intelligent (adaptive) thinning algorithms are applied to both synthetic and real data and the thinned datasets are ingested into an analysis system. The approach is motivated by the desire to better represent high-impact weather features (e. g., fronts, jets, cyclones, etc.) that are often poorly resolved in coarse-resolution forecast models and to efficiently generate a set of initial conditions that best describes the current state of the atmosphere. As a precursor to real-data applications, the algorithms are applied to one- and two-dimensional synthetic datasets. Information gleaned from the synthetic experiments is used to create a thinning algorithm that combines the best aspects of the intelligent methods (i.e., their ability to detect regions of interest) while reducing the impacts of spatial irregularities in the data. Both simple and intelligent thinning algorithms are then applied to Atmospheric Infrared Sounder (AIRS) temperature and moisture profiles. For a given retention rate, background, and observation error, the optimal 1D analyses (i.e., lowest MSE) tend to have observations that are near regions of large curvature and gradients. Observation error leads to the selection of spurious data in homogeneous regions of the intelligent algorithms. In the 2D experiments, simple thinning tends to perform better within the homogeneous data regions. Analyses produced using AIRS data demonstrate that observations selected via a combination of the simple and intelligent approaches reduce clustering, provide a more even distribution along the satellite swath edges, and, in general, have lower error and comparable computational requirements compared to standard operational thinning methodologies.
C1 [Lazarus, Steven M.; Splitt, Michael E.] Florida Inst Technol, Melbourne, FL 32901 USA.
[Lueken, Michael D.] NCEP Environm Modeling Ctr, Camp Springs, MD USA.
[Ramachandran, Rahul; Li, Xiang; Movva, Sunil; Graves, Sara J.] Univ Alabama, Informat Technol & Syst Ctr, Huntsville, AL 35899 USA.
[Zavodsky, Bradley T.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Lazarus, SM (reprint author), Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM slazarus@fit.edu
OI Splitt, Michael/0000-0002-7690-5100; Lazarus, Steven/0000-0002-5918-1059
FU NASA [NNG06GG18A]
FX This research was supported by funding under NASA Grant NNG06GG18A.
NR 36
TC 4
Z9 4
U1 0
U2 0
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
J9 WEATHER FORECAST
JI Weather Forecast.
PD JUN
PY 2010
VL 25
IS 3
BP 837
EP 851
DI 10.1175/2010WAF2222296.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 618PM
UT WOS:000279368100002
ER
PT J
AU Rozante, JR
Moreira, DS
de Goncalves, LGG
Vila, DA
AF Rozante, Jose Roberto
Moreira, Demerval Soares
de Goncalves, Luis Gustavo G.
Vila, Daniel A.
TI Combining TRMM and Surface Observations of Precipitation: Technique and
Validation over South America
SO WEATHER AND FORECASTING
LA English
DT Article
ID INTERPOLATION; SATELLITE
AB The measure of atmospheric model performance is highly dependent on the quality of the observations used in the evaluation process. In the particular case of operational forecast centers, large-scale datasets must be made available in a timely manner for continuous assessment of model results. Numerical models and surface observations usually work at distinct spatial scales (i.e., areal average in a regular grid versus point measurements), making direct comparison difficult. Alternatively, interpolation methods are employed for mapping observational data to regular grids and vice versa. A new technique (hereafter called MERGE) to combine Tropical Rainfall Measuring Mission (TRMM) satellite precipitation estimates with surface observations over the South American continent is proposed and its performance is evaluated for the 2007 summer and winter seasons. Two different approaches for the evaluation of the performance of this product against observations were tested: a cross-validation subsampling of the entire continent and another subsampling of only areas with sparse observations. Results show that over areas with a high density of observations, the MERGE technique's performance is equivalent to that of simply averaging the stations within the grid boxes. However, over areas with sparse observations, MERGE shows superior results.
C1 [Rozante, Jose Roberto; Moreira, Demerval Soares] CPTEC INPE, Ctr Weather Forecasts & Climate Studies, BR-12630000 Cachoeira Paulista, SP, Brazil.
[de Goncalves, Luis Gustavo G.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[de Goncalves, Luis Gustavo G.; Vila, Daniel A.] Univ Maryland, Earth Syst Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Vila, Daniel A.] Univ Maryland, Cooperat Inst Climate Studies, College Pk, MD 20742 USA.
RP Rozante, JR (reprint author), CPTEC INPE, Ctr Weather Forecasts & Climate Studies, Rodovia Presidente Dutra KM 40, BR-12630000 Cachoeira Paulista, SP, Brazil.
EM roberto.rozante@cptec.inpe.br
RI Vila, Daniel/G-8379-2012; de Goncalves, Luis Gustavo/G-2522-2012;
Moreira, Demerval/J-9046-2014;
OI Vila, Daniel/0000-0002-1015-5650; Moreira, Demerval/0000-0001-9147-7426;
de Goncalves, Luis Gustavo/0000-0002-1571-0916
FU FAPESP [04/09469-0]
FX The authors are grateful to the FAPESP-Serra do Mar project (04/09469-0)
and to Megan Marie Bela for helping to revise the English in this
manuscript.
NR 14
TC 39
Z9 44
U1 1
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0882-8156
EI 1520-0434
J9 WEATHER FORECAST
JI Weather Forecast.
PD JUN
PY 2010
VL 25
IS 3
BP 885
EP 894
DI 10.1175/2010WAF2222325.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 618PM
UT WOS:000279368100005
ER
PT J
AU Castillo-Rogez, JC
Schmidt, BE
AF Castillo-Rogez, Julie C.
Schmidt, B. E.
TI Geophysical evolution of the Themis family parent body
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MAIN BELT ASTEROIDS; WATER; SURFACE; BODIES; ICE; ORGANICS; ANTIOPE;
CERES
AB We model the geophysical evolution of the Themis family parent body. This study is motivated by the recent detection of water ice at the surface of 24 Themis, the first detection of free water on the surface of an asteroid. The Themis family members display a variety of spectral properties and densities, a possible indication that their parent was differentiated at the time of break-up. Differentiation of the parent body is better explained if it accreted as a mixture of ice within a few My after the production of CAIs. From these models we highlight a number of issues that provide a strong rationale for further ground-based and future space exploration of that family. Citation: Castillo-Rogez, J. C., and B. E. Schmidt (2010), Geophysical evolution of the Themis family parent body, Geophys. Res. Lett., 37, L10202, doi:10.1029/2009GL042353.
C1 [Castillo-Rogez, Julie C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schmidt, B. E.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Castillo-Rogez, JC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM julie.c.castillo@jpl.nasa.gov
OI Schmidt, Britney/0000-0001-7376-8510
FU National Aeronautics and Space Administration
FX The authors are much thankful to Andy Rivkin for his insightful comments
and valuable suggestions. Part of this work has been conducted at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Government sponsorship acknowledged.
NR 29
TC 21
Z9 21
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 29
PY 2010
VL 37
AR L10202
DI 10.1029/2009GL042353
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 603UX
UT WOS:000278234700003
ER
PT J
AU Cull, S
Arvidson, RE
Morris, RV
Wolff, M
Mellon, MT
Lemmon, MT
AF Cull, Selby
Arvidson, R. E.
Morris, R. V.
Wolff, M.
Mellon, M. T.
Lemmon, M. T.
TI Seasonal ice cycle at the Mars Phoenix landing site: 2. Postlanding
CRISM and ground observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL EMISSION SPECTROMETER; WATER-ICE; VIKING; VARIABILITY;
REFLECTANCE; ULTRAVIOLET; CAP
AB The combination of ground observations from the Mars Phoenix Lander and orbital data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) provided a detailed view of the formation of late summer surface water ice at the landing site and surrounding regions. CRISM observations of the landing site during and immediately after Phoenix operations were analyzed to track the seasonal and diurnal ice cycles during the late spring to late summer, and a nonlinear mixing model was used to estimate grain sizes and relative abundances of water ice and dust. The surface around the Phoenix landing site was ice-free from late spring through midsummer, although transient patches of mobile ices were observed in an 85 m diameter crater to the northeast of the landing site. At the similar to 10 km diameter Heimdal Crater, located similar to 10 km east of the landing site, permanent patches of water ice were observed to brighten during the late spring and darken during the summer, possibly as fine-grained water ice that was cold trapped onto the ice during late spring sintered into larger grains or finally sublimated, exposing larger-grained ice. CRISM spectra first show evidence of widespread ice during the night at solar longitude (L-s) similar to 109 degrees, similar to 9 sols before Phoenix's Surface Stereo Imager detected it. CRISM spectra first show evidence of afternoon surface ice and water ice clouds after L-s similar to 155 degrees, after Phoenix operations ended.
C1 [Cull, Selby; Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63112 USA.
[Lemmon, M. T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Mellon, M. T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Morris, R. V.] NASA, ARES, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Wolff, M.] Space Sci Inst, Boulder, CO 80301 USA.
RP Cull, S (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63112 USA.
RI Lemmon, Mark/E-9983-2010; Mellon, Michael/C-3456-2016
OI Lemmon, Mark/0000-0002-4504-5136;
FU NASA
FX We acknowledge support from NASA as part of the Phoenix and CRISM
Science Teams. We would like to thank the CRISM and HiRISE teams for
their Phoenix monitoring campaign and Hugh Kieffer and an anonymous
reviewer for their insightful reviews.
NR 43
TC 14
Z9 14
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY 29
PY 2010
VL 115
AR E00E19
DI 10.1029/2009JE003410
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 603ZO
UT WOS:000278247200001
ER
PT J
AU Ferguson, FT
Heist, RH
Nuth, JA
AF Ferguson, Frank T.
Heist, Richard H.
Nuth, Joseph A.
TI The influence of buoyant convection on the nucleation of n-propanol in
thermal diffusion cloud chambers
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
DE cloud chambers; convection; nucleation; thermal diffusion
ID CARRIER GAS-PRESSURE; HOMOGENEOUS NUCLEATION; 2-DIMENSIONAL TRANSPORT;
SUPERSATURATED VAPOR; BACKGROUND GASES; OPERATION; CONDENSATION; BINARY;
RATES; MODEL
AB A two-dimensional numerical model has been applied to three thermal diffusion cloud chamber (TDCC) investigations of n-propanol in helium taken by two different research groups to provide a quantitative example of how the results in these chambers can be affected by buoyant convection. In the first set of TDCC data, corrections for buoyancy resolve an apparent discontinuity in critical supersaturation data and also yield nucleation rate data that tend to agree better with higher rate, expansion-based studies at the same temperature. In the second TDCC study, the nucleation of propanol was studied over an extended pressure range. When the model was applied to these data, the possible variation in supersaturation values due to convection induced by conditions at the chamber sidewall was found to be comparable in magnitude to the experimentally observed range and may be responsible for some of this observed pressure dependence. In the third TDCC study, the combination of an error in a transport property and buoyant convection appear responsible for a perceived pressure effect in the experimental data. After correcting for this transport property and for buoyancy, the results at higher temperatures agree quite closely with the predictions of classical nucleation theory. (C) 2010 American Institute of Physics. [doi: 10.1063/1.3429618]
C1 [Ferguson, Frank T.] Catholic Univ Amer, Dept Chem, Washington, DC 20064 USA.
[Heist, Richard H.] Embry Riddle Aeronaut Univ, Coll Engn, Daytona Beach, FL 32114 USA.
[Nuth, Joseph A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ferguson, FT (reprint author), Catholic Univ Amer, Dept Chem, 620 Michigan Ave, Washington, DC 20064 USA.
EM frank.ferguson@nasa.gov
RI Ferguson, Frank/C-9493-2012; Nuth, Joseph/E-7085-2012
NR 48
TC 1
Z9 1
U1 0
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD MAY 28
PY 2010
VL 132
IS 20
AR 204510
DI 10.1063/1.3429618
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 603BO
UT WOS:000278183100023
PM 20515103
ER
PT J
AU Coddington, OM
Pilewskie, P
Redemann, J
Platnick, S
Russell, PB
Schmidt, KS
Gore, WJ
Livingston, J
Wind, G
Vukicevic, T
AF Coddington, O. M.
Pilewskie, P.
Redemann, J.
Platnick, S.
Russell, P. B.
Schmidt, K. S.
Gore, W. J.
Livingston, J.
Wind, G.
Vukicevic, T.
TI Examining the impact of overlying aerosols on the retrieval of cloud
optical properties from passive remote sensing
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DISCRETE-ORDINATE-METHOD; RADIATIVE-TRANSFER; EFFECTIVE RADIUS; SHIP
TRACKS; ALBEDO; STRATOCUMULUS; SENSITIVITY; SCATTERING; TRANSPORT;
ATLANTIC
AB Haywood et al. (2004) show that an aerosol layer above a cloud can cause a bias in the retrieved cloud optical thickness and effective radius. Monitoring for this potential bias is difficult because space-based passive remote sensing cannot unambiguously detect or characterize aerosol above cloud. We show that cloud retrievals from aircraft measurements above cloud and below an overlying aerosol layer are a means to test this bias. The data were collected during the Intercontinental Chemical Transport Experiment (INTEX-A) study based out of Portsmouth, New Hampshire, United States, above extensive, marine stratus cloud banks affected by industrial outflow. Solar Spectral Flux Radiometer (SSFR) irradiance measurements taken along a lower level flight leg above cloud and below aerosol were unaffected by the overlying aerosol. Along upper level flight legs, the irradiance reflected from cloud top was transmitted through an aerosol layer. We compare SSFR cloud retrievals from below-aerosol legs to satellite retrievals from the Moderate Resolution Imaging Spectroradiometer (MODIS) in order to detect an aerosol-induced bias. In regions of small variation in cloud properties, we find that SSFR and MODIS-retrieved cloud optical thickness compares within the uncertainty range for each instrument while SSFR effective radius tend to be smaller than MODIS values (by 1-2 mu m) and at the low end of MODIS uncertainty estimates. In regions of large variation in cloud properties, differences in SSFR and MODIS-retrieved cloud optical thickness and effective radius can reach values of 10 and 10 mu m, respectively. We include aerosols in forward modeling to test the sensitivity of SSFR cloud retrievals to overlying aerosol layers. We find an overlying absorbing aerosol layer biases SSFR cloud retrievals to smaller effective radii and optical thickness while nonabsorbing aerosols had no impact.
C1 [Coddington, O. M.; Pilewskie, P.; Schmidt, K. S.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Redemann, J.; Russell, P. B.; Gore, W. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Livingston, J.] SRI Int, Menlo Pk, CA 94025 USA.
[Platnick, S.; Wind, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Vukicevic, T.] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Pilewskie, P.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Redemann, J.] Bay Area Environm Res Inst, Sonoma, CA USA.
RP Coddington, OM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM odele.coddington@lasp.colorado.edu
RI Coddington, Odele/F-6342-2012; SCHMIDT, KONRAD SEBASTIAN/C-1258-2013;
Vukicevic, Tomislava/B-1386-2014; Platnick, Steven/J-9982-2014
OI Coddington, Odele/0000-0002-4338-7028; SCHMIDT, KONRAD
SEBASTIAN/0000-0003-3899-228X; Platnick, Steven/0000-0003-3964-3567
FU NASA [NNX08AI83G]; NOAA [NA06OAR4310085]
FX Numerous people contributed to the ICARTT and INTEX-A field programs. In
addition to the work provided by the people referenced in this
manuscript, we would like to thank Dan Wolfe for leading the radiosonde
effort aboard the Ronald H. Brown. We would also like to thank two
anonymous reviewers for their comments and suggestions to improve the
manuscript. This study was supported by NASA grant NNX08AI83G and NOAA
grant NA06OAR4310085.
NR 37
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U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 28
PY 2010
VL 115
AR D10211
DI 10.1029/2009JD012829
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 603VS
UT WOS:000278236800001
ER
PT J
AU de Vine, G
Ware, B
McKenzie, K
Spero, RE
Klipstein, WM
Shaddock, DA
AF de Vine, Glenn
Ware, Brent
McKenzie, Kirk
Spero, Robert E.
Klipstein, William M.
Shaddock, Daniel A.
TI Experimental Demonstration of Time-Delay Interferometry for the Laser
Interferometer Space Antenna
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID LISA
AB We report on the first demonstration of time-delay interferometry (TDI) for LISA, the Laser Interferometer Space Antenna. TDI was implemented in a laboratory experiment designed to mimic the noise couplings that will occur in LISA. TDI suppressed laser frequency noise by approximately 10(9) and clock phase noise by 6 x 10(4), recovering the intrinsic displacement noise floor of our laboratory test bed. This removal of laser frequency noise and clock phase noise in postprocessing marks the first experimental validation of the LISA measurement scheme.
C1 [de Vine, Glenn; Ware, Brent; McKenzie, Kirk; Spero, Robert E.; Klipstein, William M.; Shaddock, Daniel A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Shaddock, Daniel A.] Australian Natl Univ, Dept Phys, Canberra, ACT, Australia.
RP de Vine, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM glenn.devine@jpl.nasa.gov
RI Shaddock, Daniel/A-7534-2011
OI Shaddock, Daniel/0000-0002-6885-3494
FU National Aeronautics and Space Administration
FX This research was performed at the Jet Propulsion Laboratory (JPL),
California Institute of Technology (CIT), under contract with the
National Aeronautics and Space Administration; in part, supported by
appointments to the NASA Postdoctoral Program at JPL, administered by
Oak Ridge Associated Universities via NASA contract. The authors
acknowledge Peter Halverson, Akiko Hirai, Martin Regehr, and Andreas
Kuhnert for contributions.
NR 14
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U1 1
U2 9
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 MAY 28
PY 2010
VL 104
IS 21
AR 211103
DI 10.1103/PhysRevLett.104.211103
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 602PA
UT WOS:000278150100008
PM 20867084
ER
PT J
AU Dupont, JC
Haeffelin, M
Morille, Y
Noel, V
Keckhut, P
Winker, D
Comstock, J
Chervet, P
Roblin, A
AF Dupont, J. -C.
Haeffelin, M.
Morille, Y.
Noel, V.
Keckhut, P.
Winker, D.
Comstock, J.
Chervet, P.
Roblin, A.
TI Macrophysical and optical properties of midlatitude cirrus clouds from
four ground-based lidars and collocated CALIOP observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADIATIVE PROPERTIES; TROPICAL CIRRUS; PART III; CLIMATOLOGY; ALGORITHM;
FACILITY; MODIS; DEPOLARIZATION; RETRIEVALS; VALIDATION
AB Ground-based lidar and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) data sets gathered over four midlatitude sites, two U. S. and two French sites, are used to evaluate the consistency of cloud macrophysical and optical property climatologies that can be derived by such data sets. The consistency in average cloud height (both base and top height) between the CALIOP and ground data sets ranges from -0.4 km to +0.5 km. The cloud geometrical thickness distributions vary significantly between the different data sets, due in part to the original vertical resolutions of the lidar profiles. Average cloud geometrical thicknesses vary from 1.2 to 1.9 km, i.e., by more than 50%. Cloud optical thickness distributions in subvisible, semitransparent, and moderate intervals differ by more than 50% between ground-and space-based data sets. The cirrus clouds with optical thickness below 0.1 (not included in historical cloud climatologies) represent 30-50% of the nonopaque cirrus class. An important part of this work consists in quantifying the different possible causes of discrepancies between CALIOP and surface lidar. The differences in average cloud base altitude between ground and CALIOP data sets can be attributed to (1) irregular sampling of seasonal variations in the ground-based data, (2) day-night differences in detection capabilities by CALIOP, and (3) the restriction to situations without low-level clouds in ground-based data. Cloud geometrical thicknesses are not affected by irregular sampling of seasonal variations in the ground-based data but by the day-night differences in detection capabilities of CALIOP and by the restriction to situations without low-level clouds in ground-based data.
C1 [Dupont, J. -C.; Haeffelin, M.; Morille, Y.; Noel, V.] Ecole Polytech, IPSL, LMD, F-91128 Palaiseau, France.
[Comstock, J.] PNNL, Richland, WA 99352 USA.
[Chervet, P.; Roblin, A.] Off Natl Etud & Rech Aerosp, F-91751 Palaiseau, France.
[Keckhut, P.] Univ Versailles St Quentin, IPSL, SA, F-78280 Guyancourt, France.
[Winker, D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Dupont, JC (reprint author), Ecole Polytech, IPSL, LMD, F-91128 Palaiseau, France.
EM dupont@lmd.polytechnique.fr
RI Noel, Vincent/C-3702-2013
OI Noel, Vincent/0000-0001-9494-0340
FU Centre National d'Etudes Spatiales (CNES); Centre National de la
Recherche Scientifique (CNRS); Office National d'Etude et de Recherche
Aerospatiale (ONERA); U.S. Department of Energy; NASA
FX The authors would like to thank the Centre National d'Etudes Spatiales
(CNES), the Centre National de la Recherche Scientifique (CNRS), the
Office National d'Etude et de Recherche Aerospatiale (ONERA), and the
Climate Change Research Division of the U.S. Department of Energy as
part of the Atmospheric Radiation Measurement (ARM) Program for their
support in this study. The data at the COVE site are funded by the NASA
Earth Observing System project. We extend our acknowledgments to the
technical and computer staff of each observatory for taking the
observations and making the data set easily accessible and to the ICARE
datacenter for providing CALIOP level-2 data. The
NR 39
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U1 1
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 27
PY 2010
VL 115
AR D00H24
DI 10.1029/2009JD011943
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 603VP
UT WOS:000278236500001
ER
PT J
AU Holt, JW
Fishbaugh, KE
Byrne, S
Christian, S
Tanaka, K
Russell, PS
Herkenhoff, KE
Safaeinili, A
Putzig, NE
Phillips, RJ
AF Holt, J. W.
Fishbaugh, K. E.
Byrne, S.
Christian, S.
Tanaka, K.
Russell, P. S.
Herkenhoff, K. E.
Safaeinili, A.
Putzig, N. E.
Phillips, R. J.
TI The construction of Chasma Boreale on Mars
SO NATURE
LA English
DT Article
ID NORTH POLAR-REGION; LAYERED DEPOSITS; GEOLOGIC HISTORY; STRATIGRAPHY;
ORIGIN
AB The polar layered deposits of Mars contain the planet's largest known reservoir of water ice(1,2) and the prospect of revealing a detailed Martian palaeoclimate record(3,4), but the mechanisms responsible for the formation of the dominant features of the north polar layered deposits (NPLD) are unclear, despite decades of debate. Stratigraphic analyses of the exposed portions of Chasma Boreale-a large canyon 500 km long, up to 100 km wide, and nearly 2 km deep-have led most researchers to favour an erosional process for its formation following initial NPLD accumulation. Candidate mechanisms include the catastrophic outburst of water(5), protracted basal melting(6), erosional undercutting(7), aeolian downcutting(7-9) and a combination of these processes(10). Here we use new data from the Mars Reconnaissance Orbiter to show that Chasma Boreale is instead a long-lived, complex feature resulting primarily from non-uniform accumulation of the NPLD. The initial valley that later became Chasma Boreale was matched by a second, equally large valley that was completely filled in by subsequent deposition, leaving no evidence on the surface to indicate its former presence. We further demonstrate that topography existing before the NPLD began accumulating influenced successive episodes of deposition and erosion, resulting in most of the present-day topography. Long-term and large-scale patterns of mass balance achieved through sedimentary processes, rather than catastrophic events, ice flow or highly focused erosion, have produced the largest geomorphic anomaly in the north polar ice of Mars.
C1 [Holt, J. W.; Christian, S.] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA.
[Fishbaugh, K. E.] Smithsonian Natl Air & Space Museum, Washington, DC 20560 USA.
[Byrne, S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Christian, S.] Bryn Mawr Coll, Bryn Mawr, PA 19010 USA.
[Tanaka, K.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Russell, P. S.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Safaeinili, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Putzig, N. E.; Phillips, R. J.] SW Res Inst, Boulder, CO 80302 USA.
RP Holt, JW (reprint author), Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA.
EM jack@ig.utexas.edu
RI Holt, John/C-4896-2009; Byrne, Shane/B-8104-2012
FU Institute for Geophysics of the Jackson School of Geosciences; NASA
[NAG5-12693]; Mars Reconnaissance Orbiter (MRO); Italian Space Agency
FX We thank P. Choudhary for assistance with radar data analysis. Work at
the University of Texas was supported by the Institute for Geophysics of
the Jackson School of Geosciences, a NASA grant (NAG5-12693) to J.W.H.
and a Mars Reconnaissance Orbiter (MRO) Participating Scientist grant to
J.W.H. MRO is operated for NASA by Caltech's Jet Propulsion Laboratory.
SHARAD was provided to MRO by the Italian Space Agency through a
contract with Thales Alenia Space Italia, and is operated by the INFOCOM
Department, University of Rome. We thank the SHARAD Operations Center in
Rome for their critical support. We honour the memory of our co-author
and colleague A. S. This is UTIG contribution number 2186.
NR 26
TC 19
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U1 1
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 MAY 27
PY 2010
VL 465
IS 7297
BP 446
EP 449
DI 10.1038/nature09050
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 601FM
UT WOS:000278043700027
PM 20505721
ER
PT J
AU Kumar, M
Tsurutani, B
AF Kumar, Mohi
Tsurutani, Bruce
TI Investigations From Sun to Earth: An Interview With Bruce Tsurutani
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Kumar, Mohi] Amer Geophys Union, Washington, DC 20009 USA.
[Tsurutani, Bruce] NASA, CALTECH, Jet Prop Lab, Washington, DC 20546 USA.
RP Kumar, M (reprint author), Amer Geophys Union, Washington, DC 20009 USA.
NR 0
TC 1
Z9 1
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAY 26
PY 2010
VL 8
AR S05005
DI 10.1029/2010SW000593
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 604AH
UT WOS:000278249200001
ER
PT J
AU Cao, L
Bala, G
Caldeira, K
Nemani, R
Ban-Weiss, G
AF Cao, Long
Bala, Govindasamy
Caldeira, Ken
Nemani, Ramakrishna
Ban-Weiss, George
TI Importance of carbon dioxide physiological forcing to future climate
change
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE global warming; runoff; evapotranspiration; hydrological cycle; plant
stomata
ID STOMATAL CONDUCTANCE; CO2; PHOTOSYNTHESIS; RESPONSES; RUNOFF; PLANT;
MODEL
AB An increase in atmospheric carbon dioxide (CO(2)) concentration influences climate both directly through its radiative effect (i.e., trapping longwave radiation) and indirectly through its physiological effect (i.e., reducing transpiration of land plants). Here we compare the climate response to radiative and physiological effects of increased CO(2) using the National Center for Atmospheric Research (NCAR) coupled Community Land and Community Atmosphere Model. In response to a doubling of CO(2), the radiative effect of CO(2) causes mean surface air temperature over land to increase by 2.86 +/- 0.02 K (+/-1 standard error), whereas the physiological effects of CO(2) on land plants alone causes air temperature over land to increase by 0.42 +/- 0.02 K. Combined, these two effects cause a land surface warming of 3.33 +/- 0.03 K. The radiative effect of doubling CO(2) increases global runoff by 5.2 +/- 0.6%, primarilyby increasing precipitation over the continents. The physiological effect increases runoff by 8.4 +/- 0.6%, primarily by diminishing evapotranspiration from the continents. Combined, these two effects cause a 14.9 +/- 0.7% increase in runoff. Relative humidity remains roughly constant in response to CO(2)-radiative forcing, whereas relative humidity over land decreases in response to CO(2)-physiological forcing as a result of reduced plant transpiration. Our study points to an emerging consensus that the physiological effects of increasing atmospheric CO(2) on land plants will increase global warming beyond that caused by the radiative effects of CO(2).
C1 [Cao, Long; Caldeira, Ken; Ban-Weiss, George] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
[Bala, Govindasamy] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Bala, Govindasamy] Indian Inst Sci, Divecha Ctr Climate Change, Bangalore 560012, Karnataka, India.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Cao, L (reprint author), Carnegie Inst, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA.
EM longcao@stanford.edu
RI Caldeira, Ken/E-7914-2011;
OI Ban-Weiss, George/0000-0001-8211-2628
NR 14
TC 91
Z9 93
U1 6
U2 36
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 MAY 25
PY 2010
VL 107
IS 21
BP 9513
EP 9518
DI 10.1073/pnas.0913000107
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 601JP
UT WOS:000278054700009
PM 20445083
ER
PT J
AU Ho, CM
Morabito, DD
Woo, R
AF Ho, Christian M.
Morabito, David D.
Woo, Richard
TI Using phase scintillation spectral measurements to determine
angle-of-arrival fluctuations during solar superior conjunction
SO RADIO SCIENCE
LA English
DT Article
ID DENSITY FLUCTUATIONS; WIND
AB In this study, we develop a complete theoretical approach to derive the angle-of-arrival fluctuations (AAF) of radio signals passing through the turbulent solar plasma medium during solar superior conjunctions. Using the power spectra of phase fluctuations measured at various solar elongation angles (or impact heliocentric distances) from the Cassini spacecraft, we have defined the dependence of the AAF variance on the heliocentric distance as similar to r(-3.5) within a range very close to the Sun. This quantity decreases with increasing distance, with a slope significantly less steep than that previously expected. The AAF expression is theoretically derived by assuming a frozen turbulence and by converting a phase temporal variation into a spatial variation. To perform this calculation, the solar plasma medium is treated as an anisotropic ionized medium by applying the Booker electron irregularity spectrum model and the phase expression in term of the electron refractive index. Using the phase spectral measurements from the Cassini spacecraft during a solar superior conjunction, coefficients of the expression are calibrated, and the final AAF results are quantitatively obtained.
C1 [Ho, Christian M.; Morabito, David D.; Woo, Richard] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ho, CM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM cmho@mail.jpl.nasa.gov
FU National Aeronautics and Space Administration
FX We are indebted to Albert D. Wheelon, a CalTech trustee and pro bono
consultant to JPL, for his valuable consulting in the theoretical
aspects of the work. The authors thank Miles Sue of JPL for his comments
and suggestions. We are grateful to the referees for their valuable
review comments. 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.
NR 14
TC 0
Z9 0
U1 0
U2 2
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 MAY 25
PY 2010
VL 45
AR RS3005
DI 10.1029/2009RS004176
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 604AE
UT WOS:000278248900001
ER
PT J
AU Olaya, D
Dresselhaus, PD
Benz, SP
Herr, A
Herr, QP
Ioannidis, AG
Miller, DL
Kleinsasser, AW
AF Olaya, David
Dresselhaus, Paul D.
Benz, Samuel P.
Herr, Anna
Herr, Quentin P.
Ioannidis, Alexander G.
Miller, Donald L.
Kleinsasser, A. W.
TI Digital circuits using self-shunted Nb/NbxSi1-x/Nb Josephson junctions
SO APPLIED PHYSICS LETTERS
LA English
DT Article
DE critical current density (superconductivity); digital circuits;
Josephson effect; niobium compounds; shift registers
ID INTEGRATED-CIRCUITS; TUNNEL-JUNCTIONS; FREQUENCY; TECHNOLOGY
AB Superconducting digital circuits based on Josephson junctions with amorphous niobium-silicon (a-NbSi) barriers have been designed, fabricated, and tested. Single-flux-quantum (SFQ) shift registers operated with +/- 30% bias margins, confirming junction reproducibility and uniformity. Static digital dividers operated up to 165 GHz for a single value of bias current, which was only marginally slower than circuits fabricated with externally shunted AlOx-barrier junctions having a comparable critical current density of 4.5 kA/cm(2). In comparison, self-shunted a-NbSi junctions enabled a doubling in circuit density. This and their relatively thick 10 nm barriers could increase the yield of complex SFQ circuits. (C) 2010 American Institute of Physics. [doi:10.1063/1.3432065]
C1 [Olaya, David; Dresselhaus, Paul D.; Benz, Samuel P.] NIST, Boulder, CO 80305 USA.
[Herr, Anna; Herr, Quentin P.; Ioannidis, Alexander G.; Miller, Donald L.] Northrop Grumman Corp, Linthicum, MD 21203 USA.
[Kleinsasser, A. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Olaya, D (reprint author), NIST, Boulder, CO 80305 USA.
EM david.olaya@nist.gov
FU Defense Microelectronics Activity [H94003-04-D-0004-0091]
FX The authors acknowledge useful conversations with H. Rogalla and J.
Niemeyer, and the valuable help of G. L. Kerber at JPL. This work was
supported in part by the Defense Microelectronics Activity under
Contract No. H94003-04-D-0004-0091. U.S. government work, not subjected
to U.S. copyright.
NR 15
TC 7
Z9 8
U1 0
U2 9
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 MAY 24
PY 2010
VL 96
IS 21
AR 213510
DI 10.1063/1.3432065
PG 3
WC Physics, Applied
SC Physics
GA 603BP
UT WOS:000278183200086
ER
PT J
AU Jackson, TL
Farrell, WM
Delory, GT
Nithianandam, J
AF Jackson, Telana L.
Farrell, William M.
Delory, Gregory T.
Nithianandam, Jeyasingh
TI Martian dust devil electron avalanche process and associated
electrochemistry
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID OXIDANT ENHANCEMENT; STORMS; MARS; FIELD; GENERATION; SIMULATION;
METHANE; CLOUDS; MODEL
AB Mars' dynamic atmosphere displays localized dust devils and larger, global dust storms. Based on terrestrial analog studies, electrostatic modeling, and laboratory work, these features will contain large electrostatic fields formed via triboelectric processes. In the low-pressure Martian atmosphere, these fields may create an electron avalanche and collisional plasma due to an increase in electron density driven by the internal electrical forces. To test the hypothesis that an electron avalanche is sustained under these conditions, a self-consistent atmospheric process model is created including electron impact ionization sources and electron losses via dust absorption, electron dissociation attachment, and electron/ion recombination. This new model is called the Dust Devil Electron Avalanche Model (DDEAM). This model solves simultaneously nine continuity equations describing the evolution of the primary gaseous chemical species involved in the electrochemistry. DDEAM monitors the evolution of the electrons and primary gas constituents, including electron/water interactions. We especially focus on electron dynamics and follow the electrons as they evolve in the E field driven collisional gas. When sources and losses are self-consistently included in the electron continuity equation, the electron density grows exponentially with increasing electric field, reaching an equilibrium that forms a sustained time-stable collisional plasma. However, the character of this plasma differs depending upon the assumed growth rate saturation process (chemical saturation versus space charge). DDEAM also shows the possibility of the loss of atmospheric methane as a function of electric field due to electron dissociative attachment of the hydrocarbon. The methane destruction rates are presented and can be included in other larger atmospheric models.
C1 [Jackson, Telana L.; Farrell, William M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Delory, Gregory T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Nithianandam, Jeyasingh] Morgan State Univ, Dept Elect Engn, Baltimore, MD 21251 USA.
RP Jackson, TL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM telana.l.jackson@nasa.gov
RI Jackson, Telana/E-9102-2012; Farrell, William/I-4865-2013
FU Mars Fundamental Research Program; NASA co-op program at the Goddard
Space Flight Center
FX We gratefully acknowledge support from the Mars Fundamental Research
Program and the NASA co-op program at the Goddard Space Flight Center.
NR 31
TC 8
Z9 8
U1 0
U2 11
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 22
PY 2010
VL 115
AR E05006
DI 10.1029/2009JE003396
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 600FM
UT WOS:000277970000001
ER
PT J
AU Sim, SA
Miller, L
Long, KS
Turner, TJ
Reeves, JN
AF Sim, S. A.
Miller, L.
Long, K. S.
Turner, T. J.
Reeves, J. N.
TI Multidimensional modelling of X-ray spectra for AGN accretion disc
outflows - II
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiative transfer; methods: numerical; galaxies: active; galaxies:
individual: PG1211+143; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; RECOMBINATION RATE COEFFICIENTS; PHOTOIONIZATION
CROSS-SECTIONS; CARLO TRANSITION-PROBABILITIES; K-VACANCY STATES;
IONIZATION EQUILIBRIUM; ATOMIC DATABASE; EMISSION-LINES; ANALYTIC FITS;
AUGER DECAY
AB Highly ionized fast accretion disc winds have been suggested as an explanation for a variety of observed absorption and emission features in the X-ray spectra of active galactic nuclei. Simple estimates have suggested that these flows may be massive enough to carry away a significant fraction of the accretion energy and could be involved in creating the link between supermassive black holes and their host galaxies. However, testing these hypotheses, and quantifying the outflow signatures, requires high-quality theoretical spectra for comparison with observations. Here, we describe extensions of our Monte Carlo radiative transfer code that allow us to generate realistic theoretical spectra for a much wider variety of disc wind models than that was possible in our previous work. In particular, we have expanded the range of atomic physics simulated by the code so that L- and M-shell ions can now be included. We have also substantially improved our treatment of both ionization and radiative heating such that we are now able to compute spectra for outflows containing far more diverse plasma conditions. We present example calculations that illustrate the variety of spectral features predicted by parametrized outflow models and demonstrate their applicability to the interpretation of data by comparison with observations of the bright quasar PG1211+143. We find that the major features in the observed 2-10 keV spectrum of this object can be well reproduced by our spectra, confirming that it likely hosts a massive outflow.
C1 [Sim, S. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Miller, L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Turner, T. J.] NASA, GSFC, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 8EH, Staffs, England.
RP Sim, SA (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.
EM ssim@MPA-Garching.MPG.de
FU NASA [NNX09AO92G]
FX SAS thanks Caroline D'Angelo for many useful discussions and helpful
suggestions. TJT acknowledges NASA Grant NNX09AO92G. We thank the
anonymous referee for several constructive comments.
NR 52
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U1 1
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2010
VL 404
IS 3
BP 1369
EP 1384
DI 10.1111/j.1365-2966.2010.16396.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 592MA
UT WOS:000277381800023
ER
PT J
AU Degenaar, N
Jonker, PG
Torres, MAP
Kaur, R
Rea, N
Israel, GL
Patruno, A
Trap, G
Cackett, EM
D'Avanzo, P
Lo Curto, G
Novara, G
Krimm, H
Holland, ST
De Luca, A
Esposito, P
Wijnands, R
AF Degenaar, N.
Jonker, P. G.
Torres, M. A. P.
Kaur, R.
Rea, N.
Israel, G. L.
Patruno, A.
Trap, G.
Cackett, E. M.
D'Avanzo, P.
Lo Curto, G.
Novara, G.
Krimm, H.
Holland, S. T.
De Luca, A.
Esposito, P.
Wijnands, R.
TI Multiwavelength observations of 1RXH J173523.7-354013: revealing an
unusual bursting neutron star
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; stars: neutron; X-rays: binaries; X-rays:
bursts; X-rays: individual: 1RXH J173523; 7-354013; X-rays: individual:
IGR J17353-3539
ID X-RAY-BURSTS; JEM-X; TELESCOPE; BINARY; EXTRACTION; SUPERBURST;
EVOLUTION; SOFTWARE; MISSION; IMAGER
AB On 2008 May 14, the Burst Alert Telescope onboard the Swift mission triggered on a type-I X-ray burst from the previously unclassified ROSAT object 1RXH J173523.7-354013, establishing the source as a neutron star X-ray binary. We report on X-ray, optical and near-infrared observations of this system. The X-ray burst had a duration of similar to 2 h and belongs to the class of rare, intermediately long type-I X-ray bursts. From the bolometric peak flux of similar to 3.5 x 10-8 erg cm-2 s-1, we infer a source distance of D less than or similar to 9.5 kpc. Photometry of the field reveals an optical counterpart that declined from R = 15.9 during the X-ray burst to R = 18.9 thereafter. Analysis of post-burst Swift/X-ray Telescope observations as well as archival XMM-Newton and ROSAT data suggests that the system is persistent at a 0.5-10 keV luminosity of similar to 2 x 1035 (D/9.5 kpc)2 erg s-1. Optical and infrared photometry together with the detection of a narrow H alpha emission line (full width at half maximum = 292 +/- 9 km s-1, equivalent width = -9.0 +/- 0.4 A) in the optical spectrum confirms that 1RXH J173523.7-354013 is a neutron star low-mass X-ray binary. The H alpha emission demonstrates that the donor star is hydrogen rich, which effectively rules out that this system is an ultracompact X-ray binary.
C1 [Degenaar, N.; Kaur, R.; Rea, N.; Patruno, A.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rea, N.] ICE CSIC, IEEC, Fac Ciencias, Barcelona 08193, Spain.
[Israel, G. L.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy.
[Trap, G.] CEA Saclay, DSM, IRFU, SAp, F-91191 Gif Sur Yvette, France.
[Trap, G.] Univ Paris 07, CNRS, CEA, Observ Paris, F-75205 Paris 13, France.
[Cackett, E. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[D'Avanzo, P.; Lo Curto, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Novara, G.; De Luca, A.; Esposito, P.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy.
[Novara, G.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy.
[Krimm, H.; Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Krimm, H.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Degenaar, N (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
EM degenaar@uva.nl
RI Rea, Nanda/I-2853-2015;
OI Rea, Nanda/0000-0003-2177-6388; Israel, GianLuca/0000-0001-5480-6438; De
Luca, Andrea/0000-0001-6739-687X; Esposito, Paolo/0000-0003-4849-5092
FU Netherlands Organization for Scientific Research (NWO); Ramon y Cajal;
NASA [PF8-90052]
FX We are grateful to the referee, Craig Heinke, for useful comments that
helped improve this manuscript. This work was based on observations made
with ESO Telescopes at the Paranal and La Silla Observatories under
programme IDs: 281.D-5030(A) and 60.A9700(D) and made use of the public
data archive of Swift and INTEGRAL, as well as public data from the
XMM-Newton slew survey. Support for this work was provided by the
Netherlands Organization for Scientific Research (NWO). NR acknowledges
support from a Ramon y Cajal Research position. EMC gratefully
acknowledges support provided by NASA through the Chandra Fellowships
Program, grant number PF8-90052. We acknowledge the use of the software
package MOLLY written by Prof. Tom Marsh.
NR 56
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U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2010
VL 404
IS 3
BP 1591
EP 1602
DI 10.1111/j.1365-2966.2010.16388.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 592MA
UT WOS:000277381800043
ER
PT J
AU Keenan, FP
Milligan, RO
Jess, DB
Aggarwal, KM
Mathioudakis, M
Thomas, RJ
Brosius, JW
Davila, JM
AF Keenan, F. P.
Milligan, R. O.
Jess, D. B.
Aggarwal, K. M.
Mathioudakis, M.
Thomas, R. J.
Brosius, J. W.
Davila, J. M.
TI Emission lines of Fe xi in the 257-407 A wavelength region observed in
solar spectra from EIS/Hinode and SERTS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE atomic data; Sun: activity; Sun: corona; Sun: UV radiation
ID ULTRAVIOLET RESEARCH TELESCOPE; EFFECTIVE COLLISION STRENGTHS;
ELECTRON-IMPACT EXCITATION; EXTREME-ULTRAVIOLET; ACTIVE-REGION; ATOMIC
DATABASE; IMAGING SPECTROMETER; BEAM-FOIL; SPECTROGRAPH; INTENSITIES
AB Theoretical emission-line ratios involving Fe xi transitions in the 257-407 A wavelength range are derived using fully relativistic calculations of radiative rates and electron impact excitation cross-sections. These are subsequently compared with both long wavelength channel Extreme-Ultraviolet Imaging Spectrometer (EIS) spectra from the Hinode satellite (covering 245-291 A) and first-order observations (similar to 235-449 A) obtained by the Solar Extreme-ultraviolet Research Telescope and Spectrograph (SERTS). The 266.39, 266.60 and 276.36 A lines of Fe xi are detected in two EIS spectra, confirming earlier identifications of these features, and 276.36 A is found to provide an electron density (N(e)) diagnostic when ratioed against the 257.55 A transition. Agreement between theory and observation is found to be generally good for the SERTS data sets, with discrepancies normally being due to known line blends, while the 257.55 A feature is detected for the first time in SERTS spectra. The most useful Fe xi electron density diagnostic is found to be the 308.54/352.67 intensity ratio, which varies by a factor of 8.4 between N(e) = 108 and 1011 cm-3, while showing little temperature sensitivity. However, the 349.04/352.67 ratio potentially provides a superior diagnostic, as it involves lines which are closer in wavelength, and varies by a factor of 14.7 between N(e) = 108 and 1011 cm-3. Unfortunately, the 349.04 A line is relatively weak, and also blended with the second-order Fe x 174.52 A feature, unless the first-order instrument response is enhanced.
C1 [Keenan, F. P.; Jess, D. B.; Aggarwal, K. M.; Mathioudakis, M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Milligan, R. O.; Thomas, R. J.; Brosius, J. W.; Davila, J. M.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Lab Solar Phys, Greenbelt, MD 20771 USA.
[Brosius, J. W.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Keenan, FP (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
EM F.Keenan@qub.ac.uk
OI Jess, David/0000-0002-9155-8039
FU STFC; EPSRC; NASA [NAG5-13321]; Solar Physics Office of NASA's Space
Physics Division; AWE Aldermaston
FX DBJ and KMA acknowledge financial support from STFC and EPSRC,
respectively. ROM acknowledges support from the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Oak Ridge
Associated Universities through a contract with NASA. Hinode is a
Japanese mission developed and launched by ISAS/JAXA, collaborating with
NAOJ as a domestic partner, NASA and STFC as international partners.
Scientific operation of the Hinode mission is conducted by the Hinode
science team organized at ISAS/JAXA. Support for the post- launch
operation is provided by JAXA and NAOJ, STFC, NASA, ESA and NSC
(Norway). The SERTS rocket programme is supported by RTOP grants from
the Solar Physics Office of NASA's Space Physics Division. JWB
acknowledges additional NASA support under grant NAG5-13321. FPK is
grateful to AWE Aldermaston for the award of a William Penney
Fellowship. The authors thank Peter van Hoof for the use of his Atomic
Line List. CHIANTI is a collaborative project involving the Naval
Research Laboratory (USA), Rutherford Appleton Laboratory (UK) and the
Universities of Florence (Italy) and Cambridge (UK). We are very
grateful to the referee, Peter Young, for his comments on an earlier
version of the paper, in particular regarding the analysis of the EIS
spectra.
NR 34
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U1 0
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PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 21
PY 2010
VL 404
IS 3
BP 1617
EP 1624
DI 10.1111/j.1365-2966.2010.16389.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 592MA
UT WOS:000277381800045
ER
PT J
AU Sutton, PJ
Jones, G
Chatterji, S
Kalmus, P
Leonor, I
Poprocki, S
Rollins, J
Searle, A
Stein, L
Tinto, M
Was, M
AF Sutton, Patrick J.
Jones, Gareth
Chatterji, Shourov
Kalmus, Peter
Leonor, Isabel
Poprocki, Stephen
Rollins, Jameson
Searle, Antony
Stein, Leo
Tinto, Massimo
Was, Michal
TI X-Pipeline: an analysis package for autonomous gravitational-wave burst
searches
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID NETWORK ANALYSIS; INVERSE PROBLEM; LIGO; SIGNALS
AB Autonomous gravitational-wave searches-fully automated analyses of data that run without human intervention or assistance-are desirable for a number of reasons. They are necessary for the rapid identification of gravitational-wave burst candidates, which in turn will allow for follow-up observations by other observatories and the maximum exploitation of their scientific potential. A fully automated analysis would also circumvent the traditional 'by hand' setup and tuning of burst searches that is both labourious and time consuming. We demonstrate a fully automated search with X-Pipeline, a software package for the coherent analysis of data from networks of interferometers for detecting bursts associated with gamma-ray bursts (GRBs) and other astrophysical triggers. We discuss the methods X-Pipeline uses for automated running, including background estimation, efficiency studies, unbiased optimal tuning of search thresholds and prediction of upper limits. These are all done automatically via Monte Carlo with multiple independent data samples and without requiring human intervention. As a demonstration of the power of this approach, we apply X-Pipeline to LIGO data to compute the sensitivity to gravitational-wave emission associated with GRB 031108. We find that X-Pipeline is sensitive to signals approximately a factor of 2 weaker in amplitude than those detectable by the cross-correlation technique used in LIGO searches to date. We conclude with comments on the status of X-Pipeline as a fully autonomous, near-realtime-triggered burst search in the current LSC-Virgo Science Run.
C1 [Sutton, Patrick J.; Jones, Gareth] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Chatterji, Shourov; Stein, Leo] MIT, Cambridge, MA 02139 USA.
[Kalmus, Peter; Searle, Antony] CALTECH, Pasadena, CA 91125 USA.
[Leonor, Isabel] Univ Oregon, Eugene, OR 97403 USA.
[Poprocki, Stephen] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Rollins, Jameson] Columbia Univ, New York, NY 10027 USA.
[Tinto, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Was, Michal] Univ Paris 11, LAL, CNRS, IN2P3, Orsay, France.
RP Sutton, PJ (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
EM patrick.sutton@astro.cf.ac.uk
OI Stein, Leo/0000-0001-7559-9597
FU STFC [PP/F001096/1]; National Aeronautics and Space Administration;
California Institute of Technology; Ecole normale superieure Paris; NSF;
National Science Foundation [PHY-0107417]; [05-BEFS05-0014]
FX We thank Kipp Cannon and Ray Frey for valuable comments on an earlier
draft of this paper. PJS and GJ were supported in part by STFC grant
number PP/F001096/1. For MT, the research was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. MT was
supported under research task number 05-BEFS05-0014. MW was supported by
the California Institute of Technology and the Ecole normale superieure
Paris. LS and SP were supported by an NSF REU Site grant. We thank the
LIGO Scientific Collaboration for permission to use data from the time
of GRB 031108 for our tests. LIGO was constructed by the California
Institute of Technology and Massachusetts Institute of Technology with
funding from the National Science Foundation and operates under
cooperative agreement number PHY-0107417. This paper has been assigned
LIGO document number LIGO-P0900097-v4.
NR 46
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD MAY 21
PY 2010
VL 12
AR 053034
DI 10.1088/1367-2630/12/5/053034
PG 32
WC Physics, Multidisciplinary
SC Physics
GA 609CT
UT WOS:000278633400003
ER
PT J
AU Pugh-Thomas, D
Walsh, BM
Gupta, MC
AF Pugh-Thomas, Devin
Walsh, Brian M.
Gupta, Mool C.
TI Spectroscopy of BeAl2O4:Cr3+ with application to high-temperature
sensing
SO APPLIED OPTICS
LA English
DT Article
ID FLUORESCENCE LIFETIME; CROSS-SECTIONS; ALEXANDRITE; SENSOR; EFFICIENCY;
CRYSTALS; LASERS; ER3+; TM3+; HO3+
AB Characterization of absorption, emission, and temperature-dependent luminescent features is of significant interest for the development of optical temperature sensors and photonic devices. In this work, we conduct a comprehensive study to evaluate the orientation axis-dependent absorption and emission cross sections of Cr3+ ions in BeAl2O4. In addition, we present new data for the temperature-dependent Stark-level energies for alexandrite. Laser-induced temperature-dependent luminescence data from 300-520 K on the R-line transitions are presented for application to high-temperature sensing. (C) 2010 Optical Society of America
C1 [Pugh-Thomas, Devin; Gupta, Mool C.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
[Walsh, Brian M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Gupta, MC (reprint author), Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA.
EM mgupta@virginia.edu
FU NASA; NASA/National Institute of Aerospace (NIA)
FX The authors thank William S. Luck and William C. Edwards for their
support. We also acknowledge fellowship support from the NASA Graduate
Student Researchers program. We thank NASA/National Institute of
Aerospace (NIA) for support through the Langley Professor program.
NR 20
TC 5
Z9 6
U1 3
U2 19
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 MAY 20
PY 2010
VL 49
IS 15
BP 2891
EP 2897
DI 10.1364/AO.49.002891
PG 7
WC Optics
SC Optics
GA 599BA
UT WOS:000277883700020
PM 20490251
ER
PT J
AU Diner, DJ
Davis, A
Hancock, B
Geier, S
Rheingans, B
Jovanovic, V
Bull, M
Rider, DM
Chipman, RA
Mahler, AB
McClain, SC
AF Diner, David J.
Davis, Ab
Hancock, Bruce
Geier, Sven
Rheingans, Brian
Jovanovic, Veljko
Bull, Michael
Rider, David M.
Chipman, Russell A.
Mahler, Anna-Britt
McClain, Stephen C.
TI First results from a dual photoelastic-modulator-based polarimetric
camera
SO APPLIED OPTICS
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; POLARIZATION MODULATION; CIRCULAR-DICHROISM;
MULTIANGLE; BIREFRINGENCE; VALIDATION; SURFACES; MISR
AB We report on the construction and calibration of a dual photoelastic-modulator (PEM)-based polarimetric camera operating at 660 nm. This camera is our first prototype for a multispectral system being developed for airborne and spaceborne remote sensing of atmospheric aerosols. The camera includes a dual-PEM assembly integrated into a three-element, low-polarization reflective telescope and provides both intensity and polarization imaging. A miniaturized focal-plane assembly consisting of spectral filters and patterned wire-grid polarizers provides wavelength and polarimetric selection. A custom push-broom detector array with specialized signal acquisition, readout, and processing electronics captures the radiometric and polarimetric information. Focal-plane polarizers at orientations of 0 degrees and -45 degrees yield the normalized Stokes parameters q Q/I and u U/I respectively, which are then coregistered to obtain degree of linear polarization (DOLP) and angle of linear polarization. Laboratory test data, calibration results, and outdoor imagery acquired with the camera are presented. The results show that, over a wide range of DOLP, our challenging objective of uncertainty within +/- 0.005 has been achieved. (C) 2010 Optical Society of America
C1 [Diner, David J.; Davis, Ab; Hancock, Bruce; Geier, Sven; Rheingans, Brian; Jovanovic, Veljko; Bull, Michael; Rider, David M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chipman, Russell A.; Mahler, Anna-Britt; McClain, Stephen C.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
RP Diner, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.J.Diner@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA; University of Arizona College of Optical Sciences
under subcontract with JPL
FX We thank several colleagues for their efforts. At JPL, Nasrat Raouf
guided the development of coatings and spectral filters; Gary Gutt
designed the camera optical system; Chris Wrigley, Amy Wu, and Thomas
Cunningham assisted in design and testing of the LabMSPI electronics and
detectors; and Ghobad Saghri helped in the acquisition of imagery. At
UofA, Greg Smith, Brigit Marshall, and Brittany Lynn assisted in
building and calibrating the PSG. Brian Cairns of the Goddard Institute
for Space Studies provided comments that helped clarify parts of the
manuscript. Discussions with Craig Bohren of Pennsylvania State
University inspired a deeper appreciation of PEM history. This research
is being carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA, and at the University
of Arizona College of Optical Sciences under subcontract with JPL.
NR 33
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U1 2
U2 24
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 MAY 20
PY 2010
VL 49
IS 15
BP 2929
EP 2946
DI 10.1364/AO.49.002929
PG 18
WC Optics
SC Optics
GA 599BA
UT WOS:000277883700025
PM 20490256
ER
PT J
AU Comerford, JM
Moustakas, LA
Natarajan, P
AF Comerford, Julia M.
Moustakas, Leonidas A.
Natarajan, Priyamvada
TI OBSERVED SCALING RELATIONS FOR STRONG LENSING CLUSTERS: CONSEQUENCES FOR
COSMOLOGY AND CLUSTER ASSEMBLY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; dark matter; galaxies: clusters: individual (3C
220, A 370, Cl 0024, Cl 0939; Cl 2244, MS 0451, MS 1137, MS 2137);
galaxies: evolution; galaxies: formation; gravitational lensing: strong
ID HUBBLE-SPACE-TELESCOPE; RELAXED GALAXY CLUSTERS; X-RAY-CLUSTERS;
UNIVERSAL DENSITY PROFILE; MASS-TEMPERATURE RELATION; MEDIUM-SENSITIVITY
SURVEY; DARK-MATTER HALOS; M-T RELATION; XMM-NEWTON; DISTANT CLUSTER
AB Scaling relations of observed galaxy cluster properties are useful tools for constraining cosmological parameters as well as cluster formation histories. One of the key cosmological parameters, sigma(8), is constrained using observed clusters of galaxies, although current estimates of sigma(8) from the scaling relations of dynamically relaxed galaxy clusters are limited by the large scatter in the observed cluster mass-temperature (M-T) relation. With a sample of eight strong lensing clusters at 0.3 < z < 0.8, we find that the observed cluster concentration-mass relation can be used to reduce the M-T scatter by a factor of 6. Typically only relaxed clusters are used to estimate sigma(8), but combining the cluster concentration-mass relation with the M-T relation enables the inclusion of unrelaxed clusters as well. Thus, the resultant gains in the accuracy of sigma(8) measurements from clusters are twofold: the errors on sigma(8) are reduced and the cluster sample size is increased. Therefore, the statistics on sigma(8) determination from clusters are greatly improved by the inclusion of unrelaxed clusters. Exploring cluster scaling relations further, we find that the correlation between brightest cluster galaxy (BCG) luminosity and cluster mass offers insight into the assembly histories of clusters. We find preliminary evidence for a steeper BCG luminosity-cluster mass relation for strong lensing clusters than the general cluster population, hinting that strong lensing clusters may have had more active merging histories.
C1 [Comerford, Julia M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Natarajan, Priyamvada] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Natarajan, Priyamvada] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA.
RP Comerford, JM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
OI Moustakas, Leonidas/0000-0003-3030-2360
FU National Science Foundation; NASA [ATFP08-0169]
FX J. M. C. acknowledges support of this work by a National Science
Foundation Graduate Research Fellowship. The work of L. A. M. was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, with the support of NASA ATFP08-0169. P. N. thanks the
Radcliffe Institute for Advanced Study and the Center for Astrophysics
(CfA) for providing an intellectually stimulating atmosphere that
enabled this work.
NR 85
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U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2010
VL 715
IS 1
BP 162
EP 171
DI 10.1088/0004-637X/715/1/162
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100014
ER
PT J
AU Haghighipour, N
Vogt, SS
Butler, RP
Rivera, EJ
Laughlin, G
Meschiari, S
Henry, GW
AF Haghighipour, Nader
Vogt, Steven S.
Butler, R. Paul
Rivera, Eugenio J.
Laughlin, Greg
Meschiari, Stefano
Henry, Gregory W.
TI THE LICK-CARNEGIE EXOPLANET SURVEY: A SATURN-MASS PLANET IN THE
HABITABLE ZONE OF THE NEARBY M4V STAR HIP 57050
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; planetary systems; stars: individual (HIP 57050)
ID CARBON-DIOXIDE CLOUDS; M-CIRCLE-PLUS; M-DWARF STARS;
LUMINOSITY-RELATION; MAIN-SEQUENCE; SUPER-EARTHS; METALLICITY; CATALOG;
SEARCH; SYSTEM
AB Precision radial velocities (RV) from Keck/HIRES reveal a Saturn-mass planet orbiting the nearby M4V star HIP 57050. The planet has a minimum mass of Msin i similar to 0.3 M(J), an orbital period of 41.4 days, and an orbital eccentricity of 0.31. V-band photometry reveals a clear stellar rotation signature of the host star with a period of 98 days, well separated from the period of the RV variations and reinforcing a Keplerian origin for the observed velocity variations. The orbital period of this planet corresponds to an orbit in the habitable zone of HIP 57050, with an expected planetary temperature of similar to 230 K. The star has a metallicity of [Fe/H] = 0.32 +/- 0.06 dex, of order twice solar and among the highest metallicity stars in the immediate solar neighborhood. This newly discovered planet provides further support that the well-known planet -metallicity correlation for F, G, and K stars also extends down into the M-dwarf regime. The a priori geometric probability for transits of this planet is only about 1%. However, the expected eclipse depth is similar to 7%, considerably larger than that yet observed for any transiting planet. Though long on the odds, such a transit is worth pursuing as it would allow for high quality studies of the atmosphere via transmission spectroscopy with Hubble Space Telescope. At the expected planetary effective temperature, the atmosphere may contain water clouds.
C1 [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
[Vogt, Steven S.; Rivera, Eugenio J.; Laughlin, Greg; Meschiari, Stefano] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Butler, R. Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
RP Haghighipour, N (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
RI Butler, Robert/B-1125-2009;
OI Meschiari, Stefano/0000-0002-2930-0416
FU NASA Astrobiology Institute [NNA04CC08A, NNX09AN05G, NNX07AR40G]; NSF
[AST-0307493, AST-0908870, AST-0449986]
FX N. H. acknowledges support from the NASA Astrobiology Institute under
Cooperative Agreement NNA04CC08A at the Institute for Astronomy,
University of Hawaii, and the NASA EXOB grant NNX09AN05G. S. S. V.
gratefully acknowledges support from the NSF grants AST-0307493 and
AST-0908870, and from the NASA Keck PI program. R. P. B. gratefully
acknowledges support from the NASA OSS grant NNX07AR40G, the NASA Keck
PI program, and from the Carnegie Institution of Washington. G. L.
acknowledges support from NSF AST-0449986. G. W. H. acknowledges support
from NASA, NSF, Tennessee State University, and the state of Tennessee
through its Centers of Excellence program. We also gratefully
acknowledge the major contributions over the past decade of fellow
members of our previous California-Carnegie Exoplanet team, Geoff Marcy,
Jason Wright, Debra Fischer, and Katie Peek, in helping to obtain some
of the radial velocities presented in this paper. We are also thankful
to the anonymous referee for a careful review of our paper and his/her
suggestions that have improved our manuscript. The work herein is based
on observations obtained at theW. M. Keck Observatory, which is operated
jointly by the University of California and the California Institute of
Technology, and we thank the UH-Keck, UC-Keck and NASA-Keck Time
Assignment Committees for their support. We also extend our special
thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna
Kea we are privileged to be guests. Without their generous hospitality,
the Keck observations presented herein would not have been possible.
This research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France.
NR 43
TC 26
Z9 26
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2010
VL 715
IS 1
BP 271
EP 276
DI 10.1088/0004-637X/715/1/271
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100022
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Allafort, A
Antolini, E
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Baughman, BM
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bogart, JR
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Burnett, TH
Buson, S
Caliandro, GA
Cameron, RA
Cannon, A
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Celotti, A
Charles, E
Chekhtman, A
Chen, AW
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Costamante, L
Cotter, G
Cutini, S
D'Elia, V
Dermer, CD
de Angelis, A
de Palma, F
De Rosa, A
Digel, SW
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Escande, L
Farnier, C
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grandi, P
Grenier, IA
Grondin, MH
Grove, JE
Guiriec, S
Hadasch, D
Harding, AK
Hayashida, M
Hays, E
Healey, SE
Hill, AB
Horan, D
Hughes, RE
Iafrate, G
Itoh, R
Johannesson, G
Johnson, AS
Johnson, RP
Johnson, TJ
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Kawai, N
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lavalley, C
Lemoine-Goumard, M
Garde, ML
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Makeev, A
Malaguti, G
Massaro, E
Mazziotta, MN
McConville, W
McEnery, JE
McGlynn, S
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piranomonte, S
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Reposeur, T
Ripken, J
Ritz, S
Rodriguez, AY
Romani, RW
Roth, M
Ryde, F
Sadrozinski, HFW
Sanchez, D
Sander, A
Parkinson, PMS
Scargle, JD
Sgro, C
Shaw, MS
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Starck, JL
Stawarz, L
Strickman, MS
Suson, DJ
Tajima, H
Takahashi, H
Takahashi, T
Tanaka, T
Taylor, GB
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Ubertini, P
Uchiyama, Y
Usher, TL
Vasileiou, V
Vilchez, N
Villata, M
Vitale, V
Waite, AP
Wallace, E
Wang, P
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Allafort, A.
Antolini, E.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Baughman, B. M.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bogart, J. R.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Burnett, T. H.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Celotti, A.
Charles, E.
Chekhtman, A.
Chen, A. W.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Costamante, L.
Cotter, G.
Cutini, S.
D'Elia, V.
Dermer, C. D.
de Angelis, A.
de Palma, F.
De Rosa, A.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Escande, L.
Farnier, C.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grandi, P.
Grenier, I. A.
Grondin, M. -H.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Harding, A. K.
Hayashida, M.
Hays, E.
Healey, S. E.
Hill, A. B.
Horan, D.
Hughes, R. E.
Iafrate, G.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Johnson, R. P.
Johnson, T. J.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kawai, N.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lavalley, C.
Lemoine-Goumard, M.
Garde, M. Llena
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Makeev, A.
Malaguti, G.
Massaro, E.
Mazziotta, M. N.
McConville, W.
McEnery, J. E.
McGlynn, S.
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.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piranomonte, S.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Reposeur, T.
Ripken, J.
Ritz, S.
Rodriguez, A. Y.
Romani, R. W.
Roth, M.
Ryde, F.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Parkinson, P. M. Saz
Scargle, J. D.
Sgro, C.
Shaw, M. S.
Siskind, E. J.
Smith, P. D.
Spandre, G.
Spinelli, P.
Starck, J. -L.
Stawarz, L.
Strickman, M. S.
Suson, D. J.
Tajima, H.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Taylor, G. B.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Ubertini, P.
Uchiyama, Y.
Usher, T. L.
Vasileiou, V.
Vilchez, N.
Villata, M.
Vitale, V.
Waite, A. P.
Wallace, E.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
TI THE FIRST CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE
AREA TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; catalogs; galaxies: active; gamma rays:
galaxies
ID VLBA CALIBRATOR SURVEY; GAMMA-RAY EMISSION; ALL-SKY SURVEY; BL-LACERTAE
OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; CLASS BLAZAR SURVEY; RADIO-LOUD
AGN; SPACE-TELESCOPE; DATA RELEASE; OPTICAL IDENTIFICATIONS
AB We present the first catalog of active galactic nuclei (AGNs) detected by the Large Area Telescope (LAT), corresponding to 11 months of data collected in scientific operation mode. The First LAT AGN Catalog (1LAC) includes 671 gamma-ray sources located at high Galactic latitudes (|b| > 10 degrees) that are detected with a test statistic greater than 25 and associated statistically with AGNs. Some LAT sources are associated with multiple AGNs, and consequently, the catalog includes 709 AGNs, comprising 300 BL Lacertae objects, 296 flat-spectrum radio quasars, 41 AGNs of other types, and 72 AGNs of unknown type. We also classify the blazars based on their spectral energy distributions as archival radio, optical, and X-ray data permit. In addition to the formal 1LAC sample, we provide AGN associations for 51 low-latitude LAT sources and AGN "affiliations" (unquantified counterpart candidates) for 104 high-latitude LAT sources without AGN associations. The overlap of the 1LAC with existing gamma-ray AGN catalogs (LBAS, EGRET, AGILE, Swift, INTEGRAL, TeVCat) is briefly discussed. Various properties-such as gamma-ray fluxes and photon power-law spectral indices, redshifts, gamma-ray luminosities, variability, and archival radio luminosities-and their correlations are presented and discussed for the different blazar classes. We compare the 1LAC results with predictions regarding the gamma-ray AGN populations, and we comment on the power of the sample to address the question of the blazar sequence.
C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Roth, M.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Conrad, J.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Stawarz, L.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Labs, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Shaw, M. S.; Stawarz, L.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Atwood, W. B.; Johnson, R. P.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Johnson, R. P.; Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Axelsson, M.; Conrad, J.; Garde, M. Llena; McGlynn, S.; Ripken, J.; Ryde, F.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; 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.; Starck, J. -L.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Baughman, B. M.; Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
[Burnett, T. H.; Kerr, M.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Caliandro, G. A.; Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Cannon, A.; Celik, Oe.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cannon, A.] Univ Coll Dublin, Dublin 4, Ireland.
[Caraveo, P. A.; Chen, A. W.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Cutini, S.; D'Elia, V.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Celotti, A.] Scuola Int Super Studi Avanzati, I-34014 Trieste, Italy.
[Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA.
[Cohen-Tanugi, J.; Farnier, C.; Lavalley, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Cotter, G.] Univ Oxford, Oxford OX1 3RH, England.
[de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.; Frailis, M.] Grp Coll Udine, Sez Trieste, Ist Nazl Fis Nucl, I-33100 Udine, Italy.
[De Rosa, A.; Ubertini, P.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Dumora, D.; Escande, L.; Grondin, M. -H.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.] CEN Bordeaux Gradignan, UMR 5797, CNRS, IN2P3, F-33175 Gradignan, France.
[Dumora, D.; Escande, L.; Grondin, M. -H.; Lemoine-Goumard, M.; Lott, B.; Parent, D.; Reposeur, T.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Frailis, M.; Iafrate, G.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy.
[Fukazawa, Y.; Itoh, R.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Gehrels, N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gehrels, N.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gehrels, N.; Johnson, T. J.; McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Grandi, P.; Malaguti, G.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hadasch, D.; Torres, D. F.] ICREA, Barcelona, Spain.
[Hill, A. B.] Univ Grenoble 1, CNRS, LAOG, UMR 5571, F-38041 Grenoble 09, France.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[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.] CNRS, Ctr Etud Spatiale Rayonnements, UPS, F-31028 Toulouse 4, France.
[Massaro, E.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[McGlynn, S.; Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[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.
[Ohno, M.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Piranomonte, S.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Taylor, G. B.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Tramacere, A.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, 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 Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM elisabetta.cavazzuti@asdc.asi.it; gasparrini@asdc.asi.it;
sehealey@astro.stanford.edu; lott@cenbg.in2p3.fr; Gino.Tosti@pg.infn.it
RI Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; Funk, Stefan/B-7629-2015; 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; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
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; Morselli, Aldo/G-6769-2011; Nolan,
Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013;
Ozaki, Masanobu/K-1165-2013
OI Baldini, Luca/0000-0002-9785-7726; Gasparrini,
Dario/0000-0002-5064-9495; Villata, Massimo/0000-0003-1743-6946; Grandi,
Paola/0000-0003-1848-6013; Cutini, Sara/0000-0002-1271-2924; Axelsson,
Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; De
Rosa, Alessandra/0000-0001-5668-6863; Berenji,
Bijan/0000-0002-4551-772X; Tramacere, Andrea/0000-0002-8186-3793;
Malaguti, Giuseppe/0000-0001-9872-3378; Sgro',
Carmelo/0000-0001-5676-6214; Iafrate, Giulia/0000-0002-6185-8292;
D'Elia, Valerio/0000-0002-7320-5862; 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; Hill,
Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei,
Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018;
Funk, Stefan/0000-0002-2012-0080; 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; Torres,
Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X;
Piranomonte, Silvia/0000-0002-8875-5453; 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; Reimer,
Olaf/0000-0001-6953-1385;
FU K. A. Wallenberg Foundation; European Community [ERC-StG-200911];
International Doctorate on Astroparticle Physics (IDAPP) program;
National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie 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;
Swedish Research Council; Swedish National Space Board in Sweden;
Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes
Spatiales in France; W. M. Keck Foundation; ESO telescopes at the La
Silla Observatory [083.B-0460(B), 084.B-0711(B)]; Alfred P. Sloan
Foundation; American Museum of Natural History; Astrophysical Institute
Potsdam; University of Basel; University of Cambridge; Case Western
Reserve University; University of Chicago; Drexel University; Fermilab;
Institute for Advanced Study; Japan Participation Group; Johns Hopkins
University; Joint Institute for Nuclear Astrophysics; Kavli Institute
for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory;
Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for
Astrophysics (MPA); New Mexico State University; Ohio State University;
University of Pittsburgh; University of Portsmouth; Princeton
University; United States Naval Observatory; University of Washington;
National Science Foundation; U. S. Department of Energy; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-200911
from the European Community.; Partially supported by the International
Doctorate on Astroparticle Physics (IDAPP) program.; The Fermi LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and the
operation of the LAT as well as scientific data analysis. These include
the National Aeronautics and Space Administration and the Department of
Energy in the United States; the Commissariat a l'Energie 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.; Additional support for science analysis
during the operations phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France.; This research has made us 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. Part of this work is
based on archival data, software, or online services provided by the ASI
Science Data Center (ASDC).; Some of the results presented in this paper
are based on observations obtained with the Hobby-Eberly Telescope
(HET), a joint project of the University of Texas at Austin, the
Pennsylvania State University, Stanford University,
Ludwig-Maximilians-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 (LRS) is named for Mike Marcario of High Lonesome Optics,
who fabricated several optics for the instrument but died before its
completion. The LRS is a joint project of the Hobby-Eberly Telescope
partnership and the Instituto de Astronomia de la Universidad Nacional
Autonoma de Mexico.; This work is also partly based on optical
spectroscopy performed at the Telescopio Nazionale Galileo (TNG), La
Palma, Canary Islands (proposal AOT20/09B). These observations confirm
some of the redshifts and classifications found with the HET. We thank
the HET and TNG personnel for their assistance during the observing
runs.; The data in this paper are based partly on observations obtained
at the Hale Telescope, Palomar Observatory, as part of a collaborative
agreement between the California Institute of Technology, its divisions
Caltech Optical Observatories and the Jet Propulsion Laboratory
(operated for NASA), and Cornell University.; 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.; Some of the
data in this paper are based on observations made with ESO telescopes at
the La Silla Observatory under programs 083.B-0460(B) and
084.B-0711(B).; The National Radio Astronomy Observatory is a facility
of the National Science Foundation operated under cooperative agreement
by Associated Universities, Inc.; Funding for the Sloan Digital Sky
Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, the U. S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England. The SDSS
Web site is http://www.sdss.org/.; The SDSS is managed by the
Astrophysical Research Consortium (ARC) for the Participating
Institutions. The Participating Institutions are the American Museum of
Natural History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, The University
of Chicago, Drexel University, Fermilab, the Institute for Advanced
Study, the Japan Participation Group, The Johns Hopkins University, the
Joint Institute for Nuclear Astrophysics, the Kavli Institute for
Particle Astrophysics and Cosmology, the Korean Scientist Group, the
Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory,
the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute
for Astrophysics (MPA), New Mexico State University, Ohio State
University, University of Pittsburgh, University of Portsmouth,
Princeton University, the United States Naval Observatory, and the
University of Washington.
NR 120
TC 312
Z9 315
U1 6
U2 28
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 20
PY 2010
VL 715
IS 1
BP 429
EP 457
DI 10.1088/0004-637X/715/1/429
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100036
ER
PT J
AU Kataoka, J
Stawarz, L
Cheung, CC
Tosti, G
Cavazzuti, E
Celotti, A
Nishino, S
Fukazawa, Y
Thompson, DJ
McConville, WF
AF Kataoka, J.
Stawarz, L.
Cheung, C. C.
Tosti, G.
Cavazzuti, E.
Celotti, A.
Nishino, S.
Fukazawa, Y.
Thompson, D. J.
McConville, W. F.
TI gamma-RAY SPECTRAL EVOLUTION OF NGC 1275 OBSERVED WITH FERMI LARGE AREA
TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 1275); galaxies: jets; gamma
rays: general; radiation mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; PEAKED BL-LACERTAE; RADIO GALAXY;
PARTICLE-ACCELERATION; PERSEUS CLUSTER; SOURCE LIST; W-COMAE; EMISSION;
DISCOVERY; BLAZAR
AB We report on a detailed investigation of the high-energy gamma-ray emission from NGC 1275, a well-known radio galaxy hosted by a giant elliptical located at the center of the nearby Perseus cluster. With the increased photon statistics, the center of the gamma-ray-emitting region is now measured to be separated by only 0.46 arcmin from the nucleus of NGC 1275, well within the 95% confidence error circle with radius similar or equal to 1.5 arcmin. Early Fermi Large Area Telescope (LAT) observations revealed a significant decade-timescale brightening of NGC 1275 at GeV photon energies, with a flux about 7 times higher than the one implied by the upper limit from previous EGRET observations. With the accumulation of one year of Fermi-LAT all-sky-survey exposure, we now detect flux and spectral variations of this source on month timescales, as reported in this paper. The average > 100 MeV gamma-ray spectrum of NGC 1275 shows a possible deviation from a simple power-law shape, indicating a spectral cutoff around an observed photon energy of epsilon(gamma) = 42.2 +/- 19.6 GeV, with an average flux of F(gamma) = (2.31 +/- 0.13) x 10(-7) photons cm(-2) s(-1) and a power-law photon index, Gamma(gamma) = 2.13 +/- 0.02. The largest gamma-ray flaring event was observed in 2009 April-May and was accompanied by significant spectral variability above epsilon(gamma) greater than or similar to 1-2 GeV. The gamma-ray activity of NGC 1275 during this flare can be described by a hysteresis behavior in the flux versus photon index plane. The highest energy photon associated with the gamma-ray source was detected at the very end of the observation, with the observed energy of epsilon(gamma) = 67.4 GeV and an angular separation of about 2.4 arcmin from the nucleus. In this paper we present the details of the Fermi-LAT data analysis, and briefly discuss the implications of the observed gamma-ray spectral evolution of NGC 1275 in the context of gamma-ray blazar sources in general.
C1 [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Cheung, C. C.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Cavazzuti, E.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Celotti, A.] SISSA, I-34014 Trieste, Italy.
[Nishino, S.; Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Thompson, D. J.; McConville, W. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McConville, W. F.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Kataoka, J (reprint author), Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan.
RI Thompson, David/D-2939-2012; Tosti, Gino/E-9976-2013
OI Thompson, David/0000-0001-5217-9135;
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'EnergieAtomique; 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; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France; Polish MNiSW
[N-N203-380336]
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'EnergieAtomique 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.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.; We
acknowledge S. Digel and J. Finke for their helpful comments to improve
the manuscript. L. S. is grateful for the support from the Polish MNiSW
through the grant N-N203-380336.
NR 40
TC 37
Z9 37
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2010
VL 715
IS 1
BP 554
EP 560
DI 10.1088/0004-637X/715/1/554
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100046
ER
PT J
AU Fukumura, K
Kazanas, D
Contopoulos, I
Behar, E
AF Fukumura, Keigo
Kazanas, Demosthenes
Contopoulos, Ioannis
Behar, Ehud
TI MAGNETOHYDRODYNAMIC ACCRETION DISK WINDS AS X-RAY ABSORBERS IN ACTIVE
GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; methods: numerical;
quasars: absorption lines; X-rays: galaxies
ID GALAXY NGC-4151; BLACK-HOLES; OUTFLOWS; QUASARS; ULTRAVIOLET;
ABSORPTION; SPECTRA; DRIVEN; LINE; SIMULATIONS
AB We present the two-dimensional ionization structure of self-similarmagnetohydrodynamic winds off accretion disks around and irradiated by a central X-ray point source. On the basis of earlier observational clues and theoretical arguments, we focus our attention on a subset of these winds, namely those with radial density dependence n(r). proportional to 1/r (r is the spherical radial coordinate). We employ the photoionization code XSTAR to compute the ionic abundances of a large number of ions of different elements and then compile their line-of-sight (LOS) absorption columns. We focus our attention on the distribution of the column density of the various ions as a function of the ionization parameter xi (or equivalently r) and the angle theta. Particular attention is paid to the absorption measure distribution (AMD), namely their hydrogen-equivalent column per logarithmic xi interval, dN(H)/dlog xi, which provides a measure of the winds' radial density profiles. For the chosen density profile n(r) proportional to 1/r, the AMD is found to be independent of xi, in good agreement with its behavior inferred from the X-ray spectra of several active galactic nuclei (AGNs). For the specific wind structure and X-ray spectrum, we also compute detailed absorption line profiles for a number of ions to obtain their LOS velocities, upsilon similar to 100-300 km s(-1) (at log xi similar to 2-3) for Fe XVII and upsilon similar to 1000-4000 km s(-1) (at log xi similar to 4-5) for Fe xxv, in good agreement with the observation. Our models describe the X-ray absorption properties of these winds with only two parameters, namely the mass-accretion rate (m) over dot and the LOS angle theta. The probability of obscuration of the X-ray ionizing source in these winds decreases with increasing. m and increases steeply with the LOS inclination angle theta. As such, we concur with previous authors that these wind configurations, viewed globally, incorporate all the requisite properties of the parsec scale " torii" invoked in AGN unification schemes. We indicate that a combination of the AMD and absorption line profile observations can uniquely determine these model parameters and their bearing on AGN population demographics.
C1 [Fukumura, Keigo] Univ Maryland, Baltimore Cty UMBC CRESST, Baltimore, MD 21250 USA.
[Fukumura, Keigo; Kazanas, Demosthenes; Behar, Ehud] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Contopoulos, Ioannis] Acad Athens, Res Ctr Astron, Athens 11527, Greece.
[Behar, Ehud] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
RP Fukumura, K (reprint author), Univ Maryland, Baltimore Cty UMBC CRESST, Baltimore, MD 21250 USA.
EM Keigo.Fukumura@nasa.gov
FU NASA ADP
FX We are grateful to our anonymous referee for his/her constructive
comments that improved the manuscript. We would like to thank Tim
Kallman for his help with XSTAR incisive comments. We express our
gratitude to George Chartas for his comments on the model, and to
Takanori Sakamoto and Javier Garcia for their assistance with scripting
and running XSTAR as well as helpful comments. This work was supported
in part by NASA ADP grant.
NR 59
TC 45
Z9 45
U1 0
U2 1
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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 20
PY 2010
VL 715
IS 1
BP 636
EP 650
DI 10.1088/0004-637X/715/1/636
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100053
ER
PT J
AU Enoto, T
Rea, N
Nakagawa, YE
Makishima, K
Sakamoto, T
Esposito, P
Gotz, D
Hurley, K
Israel, GL
Kokubun, M
Mereghetti, S
Murakami, H
Nakazawa, K
Stella, L
Tiengo, A
Turolla, R
Yamada, S
Yamaoka, K
Yoshida, A
Zane, S
AF Enoto, T.
Rea, N.
Nakagawa, Y. E.
Makishima, K.
Sakamoto, T.
Esposito, P.
Goetz, D.
Hurley, K.
Israel, G. L.
Kokubun, M.
Mereghetti, S.
Murakami, H.
Nakazawa, K.
Stella, L.
Tiengo, A.
Turolla, R.
Yamada, S.
Yamaoka, K.
Yoshida, A.
Zane, S.
TI WIDE-BAND SUZAKU ANALYSIS OF THE PERSISTENT EMISSION FROM SGR 0501+4516
DURING THE 2008 OUTBURST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR 0501+4516); stars: neutron; X-rays: stars
ID X-RAY PULSARS; HIGH-ENERGY CHARACTERISTICS; XMM-NEWTON; DISCOVERY;
MAGNETARS; RXTE; TAIL
AB We observed the soft gamma repeater SGR 0501+4516 with Suzaku for similar to 51 ks on 2008 August 26-27, about 4 days after its discovery. Following the first paper, which reported on the persistent soft X-ray emission and the wide-band spectrum of an intense short burst, this paper presents an analysis of the persistent broadband (1-70 keV) spectra of this source in outburst, taken with the X-ray Imaging Spectrometer (XIS) and the Hard X-ray Detector (HXD). Pulse-phase folding in the 12-35 keV HXD-PIN data on an ephemeris based on multi-satellite timing measurements at soft X-rays revealed the pulsed signals at greater than or similar to 99% confidence in the hard X-ray band. The wide-band spectrum clearly consists of a soft component and a separate hard component, crossing over at similar to 7 keV. When the soft component is modeled by a blackbody plus a Comptonized blackbody, the hard component exhibits a 20-100 keV flux of 4.8(-0.6)(+0.8) (stat.)(-0.4)(+ 0.8) (sys.) x 10(-11) erg s(-1) cm(-2) and a photon index of Gamma = 0.79(-0.18)(+ 0.01) (sys.). The hard X-ray data are compared with those obtained by INTEGRAL about 1 day later. Combining the present results with those on other magnetars, we discuss a possible correlation between the spectral hardness of magnetars and their characteristic age and magnetic field strengths.
C1 [Enoto, T.; Makishima, K.; Nakazawa, K.; Yamada, S.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Rea, N.] Fac Ciencias, ICE CSIC, IEEC, Barcelona 08193, Spain.
[Rea, N.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Nakagawa, Y. E.; Makishima, K.] RIKEN, Cosm Radiat Lab, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
[Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Esposito, P.; Mereghetti, S.; Tiengo, A.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy.
[Esposito, P.] Ist Nazl Fis Nucl, Sez Pavia, 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.
[Turolla, R.] Univ Padua, Dept Phys, I-35131 Padua, Italy.
[Turolla, R.; Zane, S.] Univ Coll London, Mullard Space Sci Lab, 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; CNES; STFC; NASA [NNX09AI74G]; ASI/INAF [I/011/07/0]
FX We thank the Suzaku operation team for successfully carrying out the ToO
observation. We gratefully acknowledge the referee for providing
detailed comments and suggestions, which significantly improved this
paper. N.R. is supported by an NWO Veni Fellowship, D.G. thanks the CNES
for financial support, and S.Z. acknowledges support from STFC. We thank
Matthew Baring for a helpful discussion. K. H. is grateful for support
under the INTEGRAL US Guest Investigator program, NASA grant NNX09AI74G.
P. E. was supported by ASI through ASI/INAF contract I/011/07/0.
NR 31
TC 16
Z9 16
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2010
VL 715
IS 1
BP 665
EP 670
DI 10.1088/0004-637X/715/1/665
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590HM
UT WOS:000277216100056
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Bautista, M
Beilicke, M
Benbow, W
Bottcher, M
Boltuch, D
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Cui, W
Dickherber, R
Duke, C
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gibbs, K
Gillanders, GH
Godambe, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Hui, CM
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
Lamerato, A
LeBohec, S
Maier, G
McArthur, S
McCann, A
McCutcheon, M
Moriarty, P
Mukherjee, R
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Petry, D
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Roustazadeh, P
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Steele, D
Swordy, SP
Tesic, G
Theiling, M
Thibadeau, S
Varlotta, A
Vassiliev, VV
Vincent, S
Wagner, RG
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wissel, S
Wood, M
Zitzer, B
Ackermann, M
Ajello, M
Antolini, E
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Dermer, CD
de Palma, F
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Farnier, C
Favuzzi, C
Fegan, SJ
Fortin, P
Frailis, M
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giebels, B
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hays, E
Horan, D
Hughes, RE
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Garde, ML
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Makeev, A
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Omodei, N
Orlando, E
Ormes, JF
Paneque, D
Panetta, JH
Pelassa, V
Pepe, M
Pesce-Rollins, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ripken, J
Rodriguez, AY
Roth, M
Sadrozinski, HFW
Sanchez, D
Sander, A
Scargle, JD
Sgro, C
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Strickman, MS
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JB
Thayer, JG
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Usher, TL
Vasileiou, V
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Ylinen, T
Ziegler, M
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Bautista, M.
Beilicke, M.
Benbow, W.
Boettcher, M.
Boltuch, D.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Cui, W.
Dickherber, R.
Duke, C.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gibbs, K.
Gillanders, G. H.
Godambe, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Hui, C. M.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Lamerato, A.
LeBohec, S.
Maier, G.
McArthur, S.
McCann, A.
McCutcheon, M.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Petry, D.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Roustazadeh, P.
Schroedter, M.
Sembroski, G. H.
Senturk, G. Demet
Smith, A. W.
Steele, D.
Swordy, S. P.
Tesic, G.
Theiling, M.
Thibadeau, S.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Wagner, R. G.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wissel, S.
Wood, M.
Zitzer, B.
Ackermann, M.
Ajello, M.
Antolini, E.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Dermer, C. D.
de Palma, F.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Farnier, C.
Favuzzi, C.
Fegan, S. J.
Fortin, P.
Frailis, M.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giebels, B.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hays, E.
Horan, D.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Garde, M. Llena
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Makeev, A.
Mazziotta, M. N.
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.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Omodei, N.
Orlando, E.
Ormes, J. F.
Paneque, D.
Panetta, J. H.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ripken, J.
Rodriguez, A. Y.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Scargle, J. D.
Sgro, C.
Siskind, E. J.
Smith, P. D.
Spandre, G.
Spinelli, P.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. B.
Thayer, J. G.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Usher, T. L.
Vasileiou, V.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Ylinen, T.
Ziegler, M.
TI THE DISCOVERY OF gamma-RAY EMISSION FROM THE BLAZAR RGB J0710+591
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE BL Lacertae objects: individual (RGB J0710+591, VER J0710+591); gamma
rays: galaxies
ID BL-LACERTAE OBJECTS; ATMOSPHERIC CHERENKOV TELESCOPES; ACTIVE GALACTIC
NUCLEI; HOST GALAXIES; BACKGROUND-RADIATION; LAC OBJECTS; SAMPLE;
CONSTRAINTS; ASTRONOMY; VERITAS
AB The high-frequency-peaked BL Lacertae object RGB J0710+591 was observed in the very high-energy (VHE; E > 100 GeV) wave band by the VERITAS array of atmospheric Cherenkov telescopes. The observations, taken between 2008 December and 2009 March and totaling 22.1 hr, yield the discovery of VHE gamma rays from the source. RGB J0710+591 is detected at a statistical significance of 5.5 standard deviations (5.5 sigma) above the background, corresponding to an integral flux of (3.9 +/- 0.8) x 10(-12) cm(-2) s(-1) (3% of the Crab Nebula's flux) above 300 GeV. The observed spectrum can be fit by a power law from 0.31 to 4.6 TeV with a photon spectral index of 2.69 +/- 0.26(stat) +/- 0.20(sys). These data are complemented by contemporaneous multiwavelength data from the Fermi Large Area Telescope, the Swift X-ray Telescope, the Swift Ultra-Violet and Optical Telescope, and the Michigan-Dartmouth-MIT observatory. Modeling the broadband spectral energy distribution (SED) with an equilibrium synchrotron self-Compton model yields a good statistical fit to the data. The addition of an external-Compton component to the model does not improve the fit nor brings the system closer to equipartition. The combined Fermi and VERITAS data constrain the properties of the high-energy emission component of the source over 4 orders of magnitude and give measurements of the rising and falling sections of the SED.
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[Aliu, E.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Bautista, M.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Boettcher, M.; Lamerato, A.; Roustazadeh, P.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA.
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[Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
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[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Funk, S.; Glanzman, T.; Godfrey, G.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; 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.; Tibaldo, L.] Univ Paris Diderot, CNRS, Laboratoire AIM, CEA IRFU,CEA Saclay,Serv Astrophys, 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, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.; Sanchez, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
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[Celik, Oe.; Gehrels, N.; Hays, E.; Moiseev, A. A.; Thompson, D. J.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.; Moiseev, A. A.; Vasileiou, V.] CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
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[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Garde, M. Llena; Ripken, J.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dumora, D.; Lott, B.] Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France.
[Dumora, D.; Lott, B.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France.
[Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Frailis, M.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Fukazawa, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.; Vilchez, N.] UPS, CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France.
[Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[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.
[Ohno, M.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[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.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
EM jperkins@cfa.harvard.edu; fortin@llr.in2p3.fr
RI Funk, Stefan/B-7629-2015; Thompson, David/D-2939-2012; Gehrels,
Neil/D-2971-2012; Baldini, Luca/E-5396-2012; lubrano,
pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Nolan,
Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013;
Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; 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 Funk, Stefan/0000-0002-2012-0080; Thompson, David/0000-0001-5217-9135;
lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer,
Olaf/0000-0001-6953-1385; Frailis, Marco/0000-0002-7400-2135; Ward, John
E/0000-0003-1973-0794; Caraveo, Patrizia/0000-0003-2478-8018;
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; Cesarini,
Andrea/0000-0002-8611-8610; Sgro', Carmelo/0000-0001-5676-6214; Cui,
Wei/0000-0002-6324-5772; SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X
FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian
Institution; NSERC in Canada; Science Foundation Ireland; STFC in the
UK; National Aeronautics and Space Administration; Commissariat a
l'Energie 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) and Japan; Japan Aerospace Exploration Agency (JAXA)
in Japan; K.A. Wallenberg Foundation; Swedish Research Council; Swedish
National Space Board in Sweden; Istituto Nazionale di Astrofisica in
Italy; Centre National d'Etudes Spatiales in France
FX The VERITAS Collaboration acknowledges support 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. 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.; The Fermi LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and the
operation of the LAT as well as scientific data analysis. These include
the National Aeronautics and Space Administration and the Department of
Energy in the United States, the Commissariat a l'Energie 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.; Additional support for science analysis
during the operations phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France.
NR 44
TC 42
Z9 42
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAY 20
PY 2010
VL 715
IS 1
BP L49
EP L55
DI 10.1088/2041-8205/715/1/L49
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 590NM
UT WOS:000277233200011
ER
PT J
AU Mascarenhas, BS
Helenbrook, BT
Atkins, HL
AF Mascarenhas, Brendan S.
Helenbrook, Brian T.
Atkins, Harold L.
TI Coupling p-multigrid to geometric multigrid for discontinuous Galerkin
formulations of the convection-diffusion equation
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE p-Multigrid; Geometric multigrid; Discontinuous Galerkin;
Convection-diffusion equation
ID NAVIER-STOKES EQUATIONS; EULER EQUATIONS; SYSTEMS; FLOWS; GRIDS
AB An improved p-multigrid algorithm for discontinuous Galerkin (DG) discretizations of convection-diffusion problems is presented. The general p-multigrid algorithm for DG discretizations involves a restriction from the p = 1 to p = 0 discontinuous polynomial solution spaces This restriction is problematic and has limited the efficiency of the p-multigrid method For purely diffusive problems, Helenbrook and Atkins have demonstrated rapid convergence using a method that restricts from a discontinuous to continuous polynomial solution space at p = 1 It is shown that this method is not directly applicable to the convection-diffusion (CD) equation because it results in a central-difference discretization for the convective term To remedy this, Ideas from the streamwise upwind Petrov-Galerkin (SUPG) formulation are used to devise a transition from the discontinuous to continuous space at p = 1 that yields an upwind discretization The results show that the new method converges rapidly for all Peclet numbers. (C) 2010 Elsevier Inc All rights reserved.
C1 [Mascarenhas, Brendan S.] Optiwind LLC, Torrington, CT 06790 USA.
[Helenbrook, Brian T.] Clarkson Univ, Dept Mech & Aeronaut Engn, Potsdam, NY 13699 USA.
[Atkins, Harold L.] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
RP Mascarenhas, BS (reprint author), Optiwind LLC, 59 Fields St, Torrington, CT 06790 USA.
NR 21
TC 7
Z9 7
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 MAY 20
PY 2010
VL 229
IS 10
BP 3664
EP 3674
DI 10.1016/j.jcp.2010.01.020
PG 11
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 584WL
UT WOS:000276784300006
ER
PT J
AU Lyman, JM
Good, SA
Gouretski, VV
Ishii, M
Johnson, GC
Palmer, MD
Smith, DM
Willis, JK
AF Lyman, John M.
Good, Simon A.
Gouretski, Viktor V.
Ishii, Masayoshi
Johnson, Gregory C.
Palmer, Matthew D.
Smith, Doug M.
Willis, Josh K.
TI Robust warming of the global upper ocean
SO NATURE
LA English
DT Article
ID SEA-LEVEL RISE; HEAT-CONTENT; TEMPERATURE; REEVALUATION; VARIABILITY;
PROFILES; QUALITY; ARGO; XBT
AB A large (similar to 10(23) J) multi-decadal globally averaged warming signal in the upper 300 m of the world's oceans was reported roughly a decade ago(1) and is attributed to warming associated with anthropogenic greenhouse gases(2,3). The majority of the Earth's total energy uptake during recent decades has occurred in the upper ocean(3), but the underlying uncertainties in ocean warming are unclear, limiting our ability to assess closure of sea-level budgets(4-7), the global radiation imbalance(8) and climate models(5). For example, several teams have recently produced different multi-year estimates of the annually averaged global integral of upper-ocean heat content anomalies (hereafter OHCA curves) or, equivalently, the thermosteric sea-level rise(5,9-16). Patterns of inter-annual variability, in particular, differ among methods. Here we examine several sources of uncertainty that contribute to differences among OHCA curves from 1993 to 2008, focusing on the difficulties of correcting biases in expendable bathythermograph (XBT) data. XBT data constitute the majority of the in situ measurements of upper-ocean heat content from 1967 to 2002, and we find that the uncertainty due to choice of XBT bias correction dominates among-method variability in OHCA curves during our 1993-2008 study period. Accounting for multiple sources of uncertainty, a composite of several OHCA curves using different XBT bias corrections still yields a statistically significant linear warming trend for 1993-2008 of 0.64 W m(-2) (calculated for the Earth's entire surface area), with a 90-per-cent confidence interval of 0.53-0.75 W m(-2).
C1 [Lyman, John M.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Lyman, John M.; Johnson, Gregory C.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Good, Simon A.; Palmer, Matthew D.; Smith, Doug M.] Met Off Hadley Ctr, Exeter EX1 3PB, Devon, England.
[Gouretski, Viktor V.] Univ Hamburg, D-20144 Hamburg, Germany.
[Ishii, Masayoshi] Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 3050052, Japan.
[Ishii, Masayoshi] Japan Agcy Marine Earth Sci & Technol, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan.
[Willis, Josh K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lyman, JM (reprint author), Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
EM john.lyman@noaa.gov
RI Johnson, Gregory/I-6559-2012
OI Johnson, Gregory/0000-0002-8023-4020
FU US National Oceanic and Atmospheric Administration (NOAA) Climate
Program Office; NOAA; DECC/Defra [GA01101]
FX J.M.L. and G.C.J. were funded by the US National Oceanic and Atmospheric
Administration (NOAA) Climate Program Office and NOAA Research. S. A.
G., M. D. P. and D. M. S. were supported by the Joint DECC and Defra
Integrated Climate Programme DECC/Defra (GA01101). C. Domingues, S.
Levitus, T. Boyer, M. Ferrante and D. Trossman provided comments. C.
Domingues, S. Levitus, and T. Boyer also provided corrected XBT
profiles. This is Pacific Marine Environment Laboratory contribution
number 3476 and Joint Institute for Marine and Atmospheric Research
contribution number 09-372.
NR 30
TC 178
Z9 189
U1 6
U2 98
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 20
PY 2010
VL 465
IS 7296
BP 334
EP 337
DI 10.1038/nature09043
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 598IO
UT WOS:000277829200037
PM 20485432
ER
PT J
AU Sun, AY
Green, R
Rodell, M
Swenson, S
AF Sun, Alexander Y.
Green, Ronald
Rodell, Matthew
Swenson, Sean
TI Inferring aquifer storage parameters using satellite and in situ
measurements: Estimation under uncertainty
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; CLIMATE EXPERIMENT GRACE; GRAVITY RECOVERY;
TIME
AB We present a robust optimization method for estimating aquifer storage parameters (specific yield or storativity) using the Gravity Recovery and Climate Experiment (GRACE) data, in situ well level observations, and other ancillary information. Uncertainty inherent in the remotely sensed and in situ time series can adversely affect the parameter estimation process and, in the worse case, make the solution completely meaningless. Our estimation problem is formulated to directly minimize the negative impact of data uncertainty by incorporating bounds on data variations. We demonstrate our method for the interconnected Edwards- Trinity Plateau and Pecos Valley aquifers in central Texas. The study area is divided into multiple zones based on the geology and monitor well coverage. Our estimated aquifer storage parameters are consistent with previous results obtained from pumping tests and model calibration, demonstrating the potential of using GRACE data for validating regional groundwater model parameters. Citation: Sun, A. Y., R. Green, M. Rodell, and S. Swenson (2010), Inferring aquifer storage parameters using satellite and in situ measurements: Estimation under uncertainty, Geophys. Res. Lett., 37, L10401, doi: 10.1029/2010GL043231.
C1 [Sun, Alexander Y.; Green, Ronald] SW Res Inst, Geosci & Engn Div, San Antonio, TX 78238 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Swenson, Sean] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Swenson, Sean] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
RP Sun, AY (reprint author), SW Res Inst, Geosci & Engn Div, San Antonio, TX 78238 USA.
EM asun@cnwra.swri.edu
RI Rodell, Matthew/E-4946-2012; Sun, Alexander/A-9959-2011
OI Rodell, Matthew/0000-0003-0106-7437;
FU Southwest Research Institute(registered)
FX This research was funded by an internal research and development fund
from Southwest Research Institute (R). The authors wish to thank D.
Mocko at NASA for providing the NLDAS datasets, and R. Anaya and R.
Boghici at TWDB for providing the Edwards-Trinity Plateau data and for
insightful discussions.
NR 24
TC 13
Z9 13
U1 0
U2 13
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 MAY 19
PY 2010
VL 37
AR L10401
DI 10.1029/2010GL043231
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 600DA
UT WOS:000277963200005
ER
PT J
AU Cosh, MH
Tao, J
Jackson, TJ
McKee, L
O'Neill, P
AF Cosh, Michael H.
Tao, Jing
Jackson, Thomas J.
McKee, Lynn
O'Neill, Peggy
TI Vegetation water content mapping in a diverse agricultural landscape:
National Airborne Field Experiment 2006
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE Vegetation; field experimentation; thematic mapper; NDWI; agriculture
ID REMOTE-SENSING DATA; SPECTRAL INDEX; IMAGERY
AB Mapping land cover and vegetation characteristics on a regional scale is critical to soil moisture retrieval using microwave remote sensing. In aircraft-based experiments such as the National Airborne Field Experiment 2006 (NAFE'06), it is challenging to provide accurate high resolution vegetation information, especially on a daily basis. A technique proposed in previous studies was adapted here to the heterogenous conditions encountered in NAFE'06, which included a hydrologically complex landscape consisting of both irrigated and dryland agriculture. Using field vegetation sampling and ground-based reflectance measurements, the knowledge base for relating the Normalized Difference Water Index (NDWI) and the vegetation water content was extended to a greater diversity of agricultural crops, which included dryland and irrigated wheat, alfalfa, and canola. Critical to the generation of vegetation water content maps, the land cover for this region was determined from satellite visible/infrared imagery and ground surveys with an accuracy of 95.5% and a kappa coefficient of 0.95. The vegetation water content was estimated with a root mean square error of 0.33 kg/m(2). The results of this investigation contribute to a more robust database of global vegetation water content observations and demonstrate that the approach can be applied with high accuracy.
C1 [Cosh, Michael H.; Jackson, Thomas J.; McKee, Lynn] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Tao, Jing] Beijing Normal Univ, Sch Geog & Remote Sensing Sci, Beijing 100875, Peoples R China.
[O'Neill, Peggy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Cosh, MH (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
EM Michael.Cosh@ars.usda.gov; Tom.Jackson@ars.usda.gov;
Lynn.McKee@ars.usda.gov; Peggy.E.ONeill@nasa.gov
RI O'Neill, Peggy/D-2904-2013; Cosh, MIchael/A-8858-2015
OI Cosh, MIchael/0000-0003-4776-1918
NR 14
TC 1
Z9 1
U1 1
U2 15
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 MAY 19
PY 2010
VL 4
AR 043532
DI 10.1117/1.3449090
PG 10
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 602KM
UT WOS:000278138100001
ER
PT J
AU Shultz, MJ
Bisson, P
Buch, V
Groenzin, H
Li, I
AF Shultz, Mary Jane
Bisson, Patrick
Buch, Victoria
Groenzin, Henning
Li, Irene
TI Aqueous hydrogen bonding probed with polarization and matrix isolation
spectroscopy
SO JOURNAL OF MOLECULAR STRUCTURE
LA English
DT Article; Proceedings Paper
CT 18th International Conference on Horizons in Hydrogen Bond Research
CY SEP 14-18, 2009
CL Lab Leon-Brillouin CEA-CNRS, Paris, FRANCE
SP CEA Saclay, Univ Gottingen
HO Lab Leon-Brillouin CEA-CNRS
DE Ice; Water; Surface; Vibrational modes; Polarization; Sum frequency
generation
ID SUM-FREQUENCY GENERATION; LIQUID-VAPOR INTERFACE; MOLECULAR-DYNAMICS
SIMULATIONS; VIBRATIONAL SPECTROSCOPY; SALT-SOLUTIONS; WATER-SURFACE;
CARBON-TETRACHLORIDE; ROTATIONAL STRUCTURE; BINARY-SYSTEMS; IONS
AB A major challenge in hydrogen-bond research is interpreting the vibrational spectrum of water, arguably the most fundamental hydrogen bonding system. This challenge remains despite over a half century of progress in vibrational spectroscopy, largely due to a combination of the huge oscillator strength and the enormous width of the hydrogen-bond region. Lack of assignment of the resonances in the hydrogen-bond region hinders investigation of interactions between water and solutes. This lack-of-interpretation issue is an even more significant problem for studies of the aqueous interface. Numerous solutes are known to have an effect, some very dramatic, on the shape of the surface spectrum. These effects, however, are but tantalizing teasers because lack of interpretation means that the changes cannot be used to diagnose the effect of solutes or impinging gas-phase molecules on the surface.
In the reported work two techniques are used to probe the origin of vibrational resonances in the H-bonded region: the surface sensitive technique sum frequency generation (SFG) and room-temperature matrix isolation spectroscopy (RT-MIS). A polarization technique called polarization angle null (PAN) has been developed that extends SFG and enables identification of resonances. The result of applying PAN-SFG to single crystal, I(h) ice is identification of at least nine underlying resonances and assignment of two of these. One resonance is correlated with the crystal temperature and is a sensitive probe for interactions that disrupt long range order on the surface - it is a morphology reporter. The second is associated with weakly bonded, double-donor water molecules. This resonance is sensitive to interaction of hydrogen bond donors, i.e. acids, with the surface. Both modes are more correctly pictured as collective modes. These two assignments are the first definitive assignments in the hydrogen-bond region for the aqueous surface.
The effect of salts on the vibrational spectrum of water is also probed with a recently developed room-temperature, matrix-isolation technique. The matrix environment demonstrates that salts containing large anions with small cations support water-water hydrogen bonds with a vibrational resonance that has similar characteristics as the SFG spectra of salt solutions. (c) 2010 Elsevier B.V. All rights reserved.
C1 [Shultz, Mary Jane; Bisson, Patrick] Tufts Univ, Dept Chem, Pearson Lab, Medford, MA 02155 USA.
[Buch, Victoria] Hebrew Univ Jerusalem, Fritz Haber Inst Mol Dynam, IL-91904 Jerusalem, Israel.
[Groenzin, Henning] MB Technol GmbH, D-71063 Sindelfingen, Germany.
[Li, Irene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Shultz, MJ (reprint author), Tufts Univ, Dept Chem, Pearson Lab, Medford, MA 02155 USA.
EM mary.shultz@tufts.edu
OI Bisson, Patrick/0000-0002-4985-3077
NR 58
TC 4
Z9 4
U1 1
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-2860
J9 J MOL STRUCT
JI J. Mol. Struct.
PD MAY 19
PY 2010
VL 972
IS 1-3
SI SI
BP 51
EP 58
DI 10.1016/j.molstruc.2009.12.051
PG 8
WC Chemistry, Physical
SC Chemistry
GA 604VS
UT WOS:000278307200008
ER
PT J
AU Bardeen, CG
Toon, OB
Jensen, EJ
Hervig, ME
Randall, CE
Benze, S
Marsh, DR
Merkel, A
AF Bardeen, C. G.
Toon, O. B.
Jensen, E. J.
Hervig, M. E.
Randall, C. E.
Benze, S.
Marsh, D. R.
Merkel, A.
TI Numerical simulations of the three-dimensional distribution of polar
mesospheric clouds and comparisons with Cloud Imaging and Particle Size
(CIPS) experiment and the Solar Occultation For Ice Experiment (SOFIE)
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID NOCTILUCENT CLOUDS; PHYSICAL PROCESSES; OPTICAL-CONSTANTS; SUMMER
MESOSPHERE; METEORIC SMOKE; WATER-ICE; MODEL; TEMPERATURE; ATMOSPHERE;
STRATOSPHERE
AB Polar mesospheric clouds (PMC) routinely form in the cold summer mesopause region when water vapor condenses to form ice. We use a three-dimensional chemistry-climate model based on the Whole-Atmosphere Community Climate Model (WACCM) with sectional microphysics from the Community Aerosol and Radiation Model for Atmospheres (CARMA) to study the distribution and characteristics of PMCs formed by heterogeneous nucleation of water vapor onto meteoric smoke particles. We find good agreement between these simulations and cloud properties for the Northern Hemisphere in 2007 retrieved from the Solar Occultation for Ice Experiment (SOFIE) and the Cloud Imaging and Particle Size (CIPS) experiment from the Aeronomy of Ice in the Mesosphere (AIM) mission. The main discrepancy is that simulated ice number densities are less than those retrieved by SOFIE. This discrepancy may indicate an underprediction of nucleation rates in the model, the lack of small-scale gravity waves in the model, or a bias in the SOFIE results. The WACCM/CARMA simulations are not very sensitive to large changes in the barrier to heterogeneous nucleation, which suggests that large supersaturations in the model nucleate smaller meteoric smoke particles than are traditionally assumed. Our simulations are very sensitive to the temperature structure of the summer mesopause, which in the model is largely dependent upon vertically propagating gravity waves that reach the mesopause region, break, and deposit momentum. We find that cloud radiative heating is important, with heating rates of up to 8 K/d.
C1 [Bardeen, C. G.; Toon, O. B.; Randall, C. E.; Benze, S.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Bardeen, C. G.; Toon, O. B.; Randall, C. E.; Benze, S.; Merkel, A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Hervig, M. E.] GATS Inc, Driggs, ID 83422 USA.
[Jensen, E. J.] NASA, Ames Res Ctr, Moffett Field, CA 94395 USA.
[Bardeen, C. G.; Marsh, D. R.; Merkel, A.] Natl Ctr Atmospher Res, Boulder, CO 80306 USA.
RP Bardeen, CG (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
EM bardeenc@ucar.edu
RI Marsh, Daniel/A-8406-2008
OI Marsh, Daniel/0000-0001-6699-494X
FU National Science Foundation (NSF) [ATM0435713]; NASA [NNG05GQ75J,
NNX08AK45G, NNG06GE80G, NAS5-03132]; NCAR
FX The authors wish to thank Scott Bailey, Jerry Lumpe, Uwe Berger, Steve
Massie, and Doug Kinnison for their assistance. We are grateful to the
National Center for Atmospheric Research (NCAR) and the National
Aeronautics and Space Administration (NASA) for the use of computer time
to help run these simulations. We would also like to thank the SABER,
CIPS, and SOFIE science teams for the use of their data and the NCAR for
supporting our use of the WACCM model. The NCAR is operated by the
University Corporation for Atmospheric Research under the sponsorship of
the National Science Foundation (NSF). Partial support for Charles
Bardeen was provided by a NASA Earth System Science Fellowship grant
NNG05GQ75J and an NCAR Advanced Study Program Postdoctoral Fellowship.
Additional support for this project came from NASA heliophysics guest
investigator grant NNX08AK45G, NASA Aura grant NNG06GE80G, NSF grant
ATM0435713, and NASA AIM grant NAS5-03132.
NR 55
TC 21
Z9 21
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 18
PY 2010
VL 115
AR D10204
DI 10.1029/2009JD012451
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 600DQ
UT WOS:000277965100002
ER
PT J
AU Naud, CM
Chen, YH
AF Naud, Catherine M.
Chen, Yong-Hua
TI Assessment of ISCCP cloudiness over the Tibetan Plateau using
CloudSat-CALIPSO
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID HIGH-LEVEL CLOUDS; SATELLITE SOUNDERS 3I; CLIMATIC-CHANGE; IMAGERS
ISCCP; SAGE-II
AB Cloudiness over the Tibetan Plateau is difficult to estimate because ground-based measurements are sparse. Satellite observations are thus the best tool and one of the longest climatologies available, the International Satellite Cloud Climatology Project (ISCCP), relies on passive remote sensing to characterize cloud cover and altitude. Active remote sensing from space is used to assess the accuracy of the ISCCP observations over the Tibetan Plateau. August 2006 is chosen to conduct the assessment and compared to February 2007. Cloud cover from ISCCP is underestimated by about 18%, in part because of misdetection of low-level clouds at night. ISCCP cloud top pressures are overestimated by about 150-200 mb in August and 60-130 mb in February. However, the most accurate ISCCP cloud top pressures, with a maximum bias of about 50 mb, are obtained when there are thick single-layer clouds. Within the region, there is no evidence that the differences are directly dependent on elevation. Problems identified in other regions, such as multilayer clouds and optically thin clouds, explain most of the discrepancies in our study region. These results indicate that ISCCP cloud retrievals can be used to compile a realistic climatology at the highest altitudes where single-layer clouds dominate and that the retrievals are most accurate in winter.
C1 [Naud, Catherine M.; Chen, Yong-Hua] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Naud, Catherine M.; Chen, Yong-Hua] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Naud, CM (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM cnaud@giss.nasa.gov
NR 34
TC 5
Z9 5
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 18
PY 2010
VL 115
AR D10203
DI 10.1029/2009JD013053
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 600DQ
UT WOS:000277965100008
ER
PT J
AU Bera, PP
Francisco, JS
Lee, TJ
AF Bera, Partha P.
Francisco, Joseph S.
Lee, Timothy J.
TI Design strategies to minimize the radiative efficiency of global warming
molecules
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE quantum chemistry calculations; climate change; fluorocarbons; infrared
absorption; vibrational frequency
ID GAUSSIAN BASIS FUNCTIONS; FIRST-ROW ATOMS; POTENTIALS; EMISSIONS;
ANIONS; GAS
AB A strategy is devised to screen molecules based on their radiative efficiency. The methodology should be useful as one additional constraint when determining the best molecule to use for an industrial application. The strategy is based on the results of a recent study where we examined molecular properties of global warming molecules using ab initio electronic structure methods to determine which fundamental molecular properties are important in assessing the radiative efficiency of a molecule. Six classes of perfluorinated compounds are investigated. For similar numbers of fluorine atoms, their absorption of radiation in the IR window decreases according to perfluoroethers > perfluorothioethers approximate to sulfur/carbon compounds > perfluorocarbons > perfluoroolefins > carbon/nitrogen compounds. Perfluoroethers and hydrofluorethers are shown to possess a large absorption in the IR window due to (i) the C-O bonds are very polar, (ii) the C-O stretches fall within the IR window and have large IR intensity due to their polarity, and (iii) the IR intensity for C-F stretches in which the fluorine atom is bonded to the carbon that is bonded to the oxygen atom is enhanced due to a larger C-F bond polarity. Lengthening the carbon chain leads to a larger overall absorption in the IR window, though the IR intensity per bond is smaller. Finally, for a class of partially fluorinated compounds with a set number of electronegative atoms, the overall absorption in the IR window can vary significantly, as much as a factor of 2, depending on how the fluorine atoms are distributed within the molecule.
C1 [Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
[Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Francisco, JS (reprint author), Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
EM francisc@purdue.edu; Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012
FU National Aeronautics and Space Administration (NASA)
FX P. P. B. thanks Dr. Xinchuan Huang for many insightful discussions. P.
P. B. acknowledges a fellowship award from the National Aeronautics and
Space Administration (NASA) postdoctoral program administered by the Oak
Ridge Associated Universities on behalf of NASA.
NR 21
TC 9
Z9 9
U1 0
U2 11
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 MAY 18
PY 2010
VL 107
IS 20
BP 9049
EP 9054
DI 10.1073/pnas.0913590107
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 598GH
UT WOS:000277822600008
PM 20439762
ER
PT J
AU Berrilli, F
Bigazzi, A
Roselli, L
Sabatini, P
Velli, M
Alimenti, F
Cavallini, F
Greco, V
Moretti, PF
Orsini, S
Romoli, M
White, SM
AF Berrilli, F.
Bigazzi, A.
Roselli, L.
Sabatini, P.
Velli, M.
Alimenti, F.
Cavallini, F.
Greco, V.
Moretti, P. F.
Orsini, S.
Romoli, M.
White, S. M.
CA ADAHELI Team
TI The ADAHELI solar mission: Investigating the structure of Sun's lower
atmosphere
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Sun: photosphere; Sun: chromosphere; Methods: space mission
ID OPTICAL TELESCOPE; ELECTRIC-CURRENTS; TIME STRUCTURES; QUIET SUN; WAVES;
FLARE; IBIS; CHROMOSPHERE; MAGNETOGRAPH; OSCILLATIONS
AB ADAHELI (A Dvanced Astronomy for HELlophysics) is a small-class (500 kg) low-budget (50 MEuro) satellite mission for the study of the solar photosphere and the chromosphere and for monitoring solar flare emission. ADAHELI's design has completed its Phase-A feasibility study in December 2008, in the framework of ASI's (Agenzia Spaziale ltaliana) 2007 "Small Missions" Program (calling for two missions at 50 MEeuros each, plus the launch budget).
ADAHELI's main purpose is to explore Sun's lower atmosphere in the near-infrared, a region so far unexplored by solar observations from space. ADAHELI will carry out observations of the solar photosphere and of the chromosphere at high-temporal rate and high spatial and spectral resolutions.
ADAHELI will contribute to the understanding of Space Weather through the study of particle acceleration during flares. A radiometer operating in the millimeter radio band will continuously monitor the solar disk, throughout the spacecraft's life time.
ADAHELI's baseline instruments are a 50-cm high resolution telescope operating in the visible and the near-infrared, and a lightweight full-disk radiometer operating at millimeter wavelengths (90 GHz).
The core of the telescope's focal plane suite is the spectral imager based on two Fabry-Perot interferometers, flying for the first time on a solar mission. The instrument will return fast-cadence, full bi-dimensional spectral images at high-resolution, thus improving on current slit-scan, mono-dimensional architectures. Moreover, the possibility of working in polarized light will enable full 3D magnetic field reconstruction on the photosphere and the chromosphere. An optional instrumental package is also being proposed to further extend ADAHELI's scope: a full-disk telescope for helioseismology based on a double Magneto-Optical Filter, a Neutral Particle Analyzer for magnetospheric research, an Extreme Ultraviolet imaging and spectro-radiometry instrument. These options fall outside the prescribed budget.
ADAHELI, flying a Sun-Synchronous orbit at 800 km, will perform continuous, long-duration (4-h), daily acquisitions, with the possibility of extending them up to 24 h.
ADAHELI's operating life is two years, plus one extension year. Launch would be nominally planned for 2014. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Bigazzi, A.] Altran Italia SpA, I-00185 Rome, Italy.
[Berrilli, F.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Roselli, L.; Alimenti, F.] Univ Perugia, Dipartimento Ingn Elettron & Informaz, I-06125 Perugia, Italy.
[Sabatini, P.] Carlo Gavazzi Space SpA, I-20151 Milan, Italy.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Cavallini, F.] INAF Oss Astrofis Arcetri, I-50125 Florence, Italy.
[Greco, V.] INOA Ist Naz Ott Applicata, I-50125 Florence, Italy.
[Moretti, P. F.] Headquarters Consiglio Nazl Ric, I-00185 Rome, Italy.
[Orsini, S.] INAF IFSI Area Tor Vergata, I-00133 Rome, Italy.
[Romoli, M.] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy.
[White, S. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Bigazzi, A (reprint author), SERCO SpA, ESA ESRIN, Via G Galilei, I-00044 Frascati, Italy.
EM berrilli@roma2.infn.it; alberto.bigazzi@roma2.infn.it;
roselli@diei.unipg.it; psabatini@cgspace.it; velli@arcetri.astro.it;
alimenti@diei.unipg.it; fabio@arcetri.astro.it; vincenzo.greco@inoa.it;
pierfrancesco.moretti@cnr.it; stefano.orsini@ifsi-roma.inaf.it;
romoli@arcetri.astro.it; white@astro.umd.edu
RI Romoli, Marco/H-6859-2012;
OI ermolli, ilaria/0000-0003-2596-9523; CONSOLINI,
Giuseppe/0000-0002-3403-647X; ALIMENTI, Federico/0000-0002-4523-2193;
DEL MORO, DARIO/0000-0003-2500-5054; Cauzzi, Gianna/0000-0002-6116-7301;
Romano, Paolo/0000-0001-7066-6674; Di Mauro, Maria
Pia/0000-0001-7801-7484
NR 37
TC 17
Z9 17
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 MAY 17
PY 2010
VL 45
IS 10
BP 1191
EP 1202
DI 10.1016/j.asr.2010.01.026
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 598RX
UT WOS:000277857000001
ER
PT J
AU Esplin, TL
Cable, ML
Gray, HB
Ponce, A
AF Esplin, Taran L.
Cable, Morgan L.
Gray, Harry B.
Ponce, Adrian
TI Terbium-Macrocycle Complexes as Chemical Sensors: Detection of an
Aspirin Metabolite in Urine Using a Salicylurate-Specific Receptor Site
SO INORGANIC CHEMISTRY
LA English
DT Article
ID ELECTRONIC ENERGY LEVELS; LANTHANIDE AQUO IONS; INTRAMOLECULAR
PROTON-TRANSFER; GENTISIC ACID; CAPILLARY-ELECTROPHORESIS;
2-HYDROXYHIPPURIC ACID; LIQUID-CHROMATOGRAPHY; ACETYLSALICYLIC-ACID;
SALICYLATE; STATE
AB Salicylurate (SU) is the major metabolite in urine of acetylsalicylic acid (aspirin) and can be used as a metric to monitor aspirin pharmacokinetics and as an indicator of appendicitis, anemia, and liver disease. Detection in urine and plasma currently requires solvent extraction or other sample handling prior to analysis. We present a simple method to quantify SU in urine via chelation to a terbium binary complex with the macrocycle 1,4,7,10-tetraazacyclododecane-1,7-bisacetate (DO2A). Binding of SU to form the [Tb(DO2A)(SU)](-) ternary complex triggers intense luminescence under UV excitation due to an absorbance-energy transfer-emission mechanism. Here we report characterization of the [Tb(DO2A)(SU)](-) ternary complex and application of this sensitized lanthanide luminescence method to quantify SU in urine samples following a low-dose aspirin regimen,
C1 [Esplin, Taran L.; Cable, Morgan L.; Ponce, Adrian] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA.
[Cable, Morgan L.; Gray, Harry B.; Ponce, Adrian] CALTECH, Beckman Inst, Pasadena, CA 91125 USA.
RP Ponce, A (reprint author), CALTECH, Jet Prop Lab, Planetary Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ponce@caltech.edu
FU Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautic and Space Administration; NASA
Astrobiology and Planetary Protection Programs (A.P.); Department of
Homeland Security Chemical and Biological Research & Development
Program; NIH; NSF; Arnold and Mabel Beckman Foundation
FX The authors thank Mona Shahgholi for assistance with mass spectrometry.
This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautic and Space Administration and was sponsored by the NASA
Astrobiology and Planetary Protection Programs (A.P.), the Department of
Homeland Security Chemical and Biological Research & Development Program
(A.P.), the NASA Graduate Student Research Program (M.L.C.), and the
NASA Undergraduate Student Research Program (T.L.E.). Work at the
Beckman Institute was supported by the NIH, NSF, and the Arnold and
Mabel Beckman Foundation (H.B.G.).
NR 39
TC 19
Z9 19
U1 0
U2 10
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0020-1669
J9 INORG CHEM
JI Inorg. Chem.
PD MAY 17
PY 2010
VL 49
IS 10
BP 4643
EP 4647
DI 10.1021/ic1003066
PG 5
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA 592MS
UT WOS:000277383900034
PM 20405964
ER
PT J
AU Lee, J
Kim, J
Song, CH
Ryu, JH
Ahn, YH
Song, CK
AF Lee, Jaehwa
Kim, Jhoon
Song, Chul H.
Ryu, Joo-Hyung
Ahn, Yu-Hwan
Song, C. K.
TI Algorithm for retrieval of aerosol optical properties over the ocean
from the Geostationary Ocean Color Imager
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Remote sensing; Algorithm; Aerosol optical depth; Fine-mode fraction;
Aerosol type; Geostationary
ID VALIDATION; MTSAT-1R; CHANNELS; AVHRR
AB An aerosol retrieval algorithm for the first Geostationary Ocean Color Imager (GOCI) to be launched in March 2010 onboard the Communication, Ocean, and Meteorological Satellite (COMS) is presented. The algorithm retrieves aerosol optical depth (AOD), fine-mode fraction (FMIF), and aerosol type in 500 m x 500 m resolution. All the products are retrieved over clear water which is defined by surface reflectance ratio between 640 nm and 860 nm (SRR) less or equal to 2.5, while only AOD is retrieved over turbid water (SRR>2.5) due to high surface reflectance. To develop optimized algorithm for the target area of GOCI, optical properties of aerosol are analyzed from extensive observation of AERONET sunphotometers to generate lookup table. Surface reflectance of turbid water is determined from 30-day composite of Rayleigh- and gas corrected reflectance. By applying the present algorithm to MODIS top-of-the atmosphere reflectance, three different aerosol cases dominated by anthropogenic aerosol contains black carbon (BC), dust, and non-absorbing aerosol are analyzed to test the algorithm. The algorithm retrieves AOD, and size information together with aerosol type which are consistent with results inferred by RGB image in a qualitative way. The comparison of the retrieved AOD with those of MODIS collection 5 and AERONET sunphotometer observations shows reliable results. Especially, the application of turbid water algorithm significantly increases the accuracy in retrieving AOD at Anmyon station. The sensitivity study between MODIS and GOCI instruments in terms of relative sensitivity and scattering angle shows promising applicability of the present algorithm to future GOCI measurements. (C) 2010 Elsevier Inc. All rights reserved.
C1 [Lee, Jaehwa; Kim, Jhoon] Yonsei Univ, Dept Atmospher Sci, Brain Korea Program 21, Inst Earth Astron & Atmosphere, Seoul 120749, South Korea.
[Song, Chul H.] GIST, Dept Environm Engn, Gwangiu, South Korea.
Korea Ocean Res & Dev Inst, Ocean Satellite Res Grp, Ansan, South Korea.
[Lee, Jaehwa; Kim, Jhoon] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA USA.
[Lee, Jaehwa; Kim, Jhoon] NASA, Aerosol & Cloud Grp, JPL, Pasadena, CA USA.
[Song, C. K.] Natl Inst Environm Res, Inchon, South Korea.
RP Kim, J (reprint author), Yonsei Univ, Dept Atmospher Sci, Brain Korea Program 21, Inst Earth Astron & Atmosphere, Seoul 120749, South Korea.
EM jkim2@yonsei.ac.kr
RI Kwon, Yulee/B-8433-2009; Song, Chang-Keun/S-2255-2016
OI Kwon, Yulee/0000-0002-6515-9181; Song, Chang-Keun/0000-0002-8811-2626
FU Korean Ocean Research and Development Institute (KORDI); Korea
Meteorological Administration Research and Development Program [CATER
2006-3203]; Brain Korea 21 (BK21)
FX We thank the Korean Ocean Research and Development Institute (KORDI) for
the development and application of GOCI in this work. This work was
funded by the Korea Meteorological Administration Research and
Development Program under grant CATER 2006-3203. This research was
partially supported by the Brain Korea 21 (BK21) program for J. Kim and
J. Lee. We also thank the principal investigators and their staff for
establishing and maintaining the AERONET sites.
NR 25
TC 29
Z9 31
U1 6
U2 26
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD MAY 17
PY 2010
VL 114
IS 5
BP 1077
EP 1088
DI 10.1016/j.rse.2009.12.021
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 571UH
UT WOS:000275780800013
ER
PT J
AU Heimann, A
Johnson, CM
Beard, BL
Valley, JW
Roden, EE
Spicuzza, MJ
Beukes, NJ
AF Heimann, Adriana
Johnson, Clark M.
Beard, Brian L.
Valley, John W.
Roden, Eric E.
Spicuzza, Michael J.
Beukes, Nicolas J.
TI Fe, C, and O isotope compositions of banded iron formation carbonates
demonstrate a major role for dissimilatory iron reduction in similar to
2.5 Ga marine environments
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Fe; isotopes; BIF; Kuruman; carbonates; Archean/Paleoproterozoic
ID RARE-EARTH-ELEMENTS; PROTEROZOIC TRANSVAAL SUPERGROUP; AMORPHOUS FERRIC
HYDROXIDE; WESTERN-AUSTRALIA; SOUTH-AFRICA; FE(III) REDUCTION; OXIDE
REDUCTION; MICROBIAL CARBONATE; DIAGENETIC SIDERITE; FACIES TRANSITION
AB Combined Fe, C, and O isotope measurements of similar to 2.5 Ga banded iron formation (BIF) carbonates from the Kuruman Iron Formation and underlying BIF and platform Ca-Mg carbonates of the Gamohaan Formation, South Africa, constrain the biologic and abiologic formation pathways in these extensive BIF deposits. Vertical intervals of up to 100 m were sampled in three cores that cover a lateral extent of similar to 250 km. BIF Fe carbonates have significant Fe isotope variability (delta(56)Fe = +1 to 1 parts per thousand) and relatively low delta(13)C (down to - 12 parts per thousand) and 6180 values (delta(18)O -+ 21 parts per thousand). In contrast, Gamohaan and stratigraphically-equivalent Campbellrand Ca-Mg carbonates have near-zero delta(13)C values and higher delta(18)O values. These findings argue against siderite precipitation from seawater as the origin of BIF Fe-rich carbonates. Instead, the C, O, and Fe isotope compositions of BIF Fe carbonates reflect authigenic pathways of formation in the sedimentary pile prior to lithification, where microbial dissimilatory iron reduction (DIR) was the major process that controlled the C, O, and Fe isotope compositions of siderite. Isotope mass-balance reactions indicate that the low-delta(13)C and low-delta(18)O values of BIF siderite, relative to those expected for precipitation from seawater, reflect inheritance of C and O isotope compositions of precursor organic carbon and ferric hydroxide that were generated in the photic zone and deposited on the seafloor. Carbon-Fe isotope relations suggest that BIF Fe carbonates formed through two end-member pathways: low-delta(13)C, low-delta(56)Fe Fe carbonates formed from remobilized, low-delta(56)Fe aqueous Fe(2+) produced by partial DIR of iron oxide, whereas low-delta(13)C, high-delta(56)Fe Fe carbonates formed by near-complete DIR of high-delta(56)Fe iron oxides that were residual from prior partial DIR. An important observation is the common occurrence of iron oxide inclusions in the high-delta(56)Fe siderite, supporting a model where such compositions reflect DIR "in place" in the soft sediment In contrast, the isotopic composition of low-Fe carbonates in limestone/dolomite may constitute a record of seawater environments, although our petrographic studies indicate that the presence of pyrite in most low-Fe carbonates may influence the Fe isotope compositions. The combined Fe, C, and O isotope data from Kuruman BIF carbonates indicate that BIF siderites that have negative, near-zero, or positive delta(56)Fe values may all record biological Fe cycling, where the range in delta(56)Fe values records differential Fe mobilization via DIR in the sediment prior to lithification. Our results demonstrate that the inventory of low-delta(56)Fe marine sedimentary rocks of Neoarchean to Paleoproterozoic age, although impressive in volume, may represent only a minimum of the total inventory of Fe that was cycled by bacteria. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Heimann, Adriana] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA.
[Heimann, Adriana; Johnson, Clark M.; Beard, Brian L.; Valley, John W.; Roden, Eric E.; Spicuzza, Michael J.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Heimann, Adriana; Johnson, Clark M.; Beard, Brian L.; Valley, John W.; Roden, Eric E.; Spicuzza, Michael J.] NASA, Astrobiol Inst, Washington, DC USA.
[Beukes, Nicolas J.] Univ Johannesburg, Dept Geol, Johannesburg, South Africa.
RP Heimann, A (reprint author), E Carolina Univ, Dept Geol Sci, 101 Graham Bldg, Greenville, NC 27858 USA.
EM heimanna@ecu.edu
RI Valley, John/B-3466-2011
OI Valley, John/0000-0003-3530-2722
FU NASA Astrobiology Institute; National Science Foundation
FX We thank John Fournelle for his help with electron microprobe, SEM, and
EBSD determinations and Hiromi Konishi and Huifang Xu for performing
preliminary TEM analysis. We thank Max Coleman for useful discussions.
Journal reviews by editor Rick Carlson, Balz Kamber, and an anonymous
reviewer helped to improve the manuscript. This research was funded by
the NASA Astrobiology Institute and the National Science Foundation.
NR 89
TC 71
Z9 75
U1 7
U2 75
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAY 15
PY 2010
VL 294
IS 1-2
BP 8
EP 18
DI 10.1016/j.epsl.2010.02.015
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 607LS
UT WOS:000278506200002
ER
PT J
AU Kappler, A
Johnson, CM
Crosby, HA
Beard, BL
Newman, DK
AF Kappler, A.
Johnson, C. M.
Crosby, H. A.
Beard, B. L.
Newman, D. K.
TI Evidence for equilibrium iron isotope fractionation by nitrate-reducing
iron(II)-oxidizing bacteria
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID FE(II)-OXIDIZING PHOTOAUTOTROPHIC BACTERIA; PHOTOTROPHIC FE(II)
OXIDATION; DISSIMILATORY FE(III); AQUEOUS FE(II); FERROUS IRON;
CIRCUMNEUTRAL PH; FE; REDUCTION; HEMATITE; GEOCHEMISTRY
AB Iron isotope fractionations produced during chemical and biological Fe(II) oxidation are sensitive to the proportions and nature of dissolved and solid-phase Fe species present, as well as the extent of isotopic exchange between precipitates and aqueous Fe. Iron isotopes therefore potentially constrain the mechanisms and pathways of Fe redox transformations in modern and ancient environments. In the present study, we followed in batch experiments Fe isotope fractionations between Fe(II)(aq) and Fe(III) oxide/hydroxide precipitates produced by the Fe(III) mineral encrusting, nitrate-reducing, Fe(II)-oxidizing Acidovorax sp. strain BoFeN1. Isotopic fractionation in (56)Fe/(54)Fe approached that expected for equilibrium conditions, assuming an equilibrium Delta(56)Fe(Fe(OH)3-Fe(II)aq) fractionation factor of +3.0 parts per thousand. Previous studies have shown that Fe(II) oxidation by this Acidovorax strain occurs in the periplasm, and we propose that Fe isotope equilibrium is maintained through redox cycling via coupled electron and atom exchange between Fe(II)(aq) and Fe(III) precipitates in the contained environment of the periplasm. In addition to the apparent equilibrium isotopic fractionation, these experiments also record the kinetic effects of initial rapid oxidation, and possible phase transformations of the Fe(III) precipitates. Attainment of Fe isotope equilibrium between Fe(III) oxide/hydroxide precipitates and Fe(II)(aq) by neutrophilic, Fe(II)-oxidizing bacteria or through abiologic Fe(II)(aq) oxidation is generally not expected or observed, because the poor solubility of their metabolic product, i.e. Fe(III), usually leads to rapid precipitation of Fe(III) minerals, and hence expression of a kinetic fractionation upon precipitation; in the absence of redox cycling between Fe(II)(aq) and precipitate, kinetic isotope fractionations are likely to be retained. These results highlight the distinct Fe isotope fractionations that are produced by different pathways of biological and abiological Fe(II) oxidation. (c) 2010 Elsevier Ltd. All rights reserved.
C1 [Kappler, A.; Newman, D. K.] CALTECH, GPS Div, Pasadena, CA 91125 USA.
[Johnson, C. M.; Crosby, H. A.; Beard, B. L.] Univ Wisconsin, Dept Geol & Geophys, Madison, WI 53706 USA.
[Johnson, C. M.; Beard, B. L.] Univ Wisconsin, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Kappler, A (reprint author), Univ Tubingen, Ctr Appl Geosci, D-72076 Tubingen, Germany.
EM andreas.kappler@uni-tuebingen.de
RI Kappler, Andreas/G-7221-2016;
OI Crosby, Heidi/0000-0002-0360-0779
FU German Research Foundation (DFG); Packard Foundation; NASA Astrobiology
Institute; National Science Foundation
FX The research was supported by a post-doc fellowship and an Emmy-Noether
fellowship from the German Research Foundation (DFG) to A.K. and a grant
from the Packard Foundation to D.K.N. Additional funding from the NASA
Astrobiology Institute supported C.M.J. and B.L.B., and funding from the
National Science Foundation supported B.L.B. and H.A.C. We would like to
thank Ma Chi (Caltech) for help with the XRD. Sebastian Schaedler
(University of Tuebingen) and Claus Burkhardt (NMI Reutlingen) are
acknowledged for providing scanning electron micrographs. D.K.N. is an
Investigator of the Howard Hughes Medical Institute. We thank AE Stephan
Kraemer, Thomas Bullen, and an anonymous reviewer, whose comments helped
improve the manuscript.
NR 53
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U1 6
U2 53
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 MAY 15
PY 2010
VL 74
IS 10
BP 2826
EP 2842
DI 10.1016/j.gca.2010.02.017
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 587JZ
UT WOS:000276989400002
ER
PT J
AU Dyudina, UA
Ingersoll, AP
Ewald, SP
Porco, CC
Fischer, G
Kurth, WS
West, RA
AF Dyudina, U. A.
Ingersoll, A. P.
Ewald, S. P.
Porco, C. C.
Fischer, G.
Kurth, W. S.
West, R. A.
TI Detection of visible lightning on Saturn
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID CASSINI IMAGING SCIENCE; MOIST CONVECTION; ELECTROSTATIC DISCHARGES;
GALILEO IMAGES; GIANT PLANETS; JUPITER; ATMOSPHERE; CLOUDS; STORMS;
MODEL
AB Until now, evidence for lightning on Saturn has been indirect - through radio emissions and cloud morphology. Here we report the first visible detection of lightning, on the night side on August 17, 2009 at -36.4 degrees +/- 0.1 degrees planetocentric latitude and 10.6 degrees +/- 0.9 degrees west longitude. No other locations produced lightning detectable by either imaging or radio. The lightning images are consistent with a single cloud flashing once per minute. The visible energy of a single flash is comparable to that on Earth and Jupiter, and ranges up to 1.7 x 10(9) Joules. The diameter of the lightning flashes is similar to 200 km, which suggests the lightning is 125-250 km below cloud tops. This depth is above the base of the liquid H(2)O-NH(3) cloud and may be either in the NH(4)SH cloud or in the H(2)O ice cloud. Saturn's lower internal heat transport and likely 5-10 fold enrichment of water largely explain the lower occurrence rate of moist convection on Saturn relative to Jupiter. Citation: Dyudina, U. A., A. P. Ingersoll, S. P. Ewald, C. C. Porco, G. Fischer, W. S. Kurth, and R. A. West (2010), Detection of visible lightning on Saturn, Geophys. Res. Lett., 37, L09205, doi: 10.1029/2010GL043188.
C1 [Fischer, G.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria.
[Kurth, W. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Porco, C. C.] Space Sci Inst, Cassini Imaging Cent Lab Operat, Boulder, CO 80301 USA.
[Dyudina, U. A.; Ingersoll, A. P.; Ewald, S. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Dyudina, UA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM ulyana@gps.caltech.edu
FU NASA; Austrian Science Fund [P21295-N16]
FX This research was supported by the NASA Cassini Project. G. F.
acknowledges support from the Austrian Science Fund FWF under the
project P21295-N16. We thank J. Burns for commentson the manuscript.
U.A.D. thanks P. Nicholson for estimates of ring brightness during the
equinox needed for planning these observations.
NR 31
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U1 1
U2 7
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 MAY 15
PY 2010
VL 37
AR L09205
DI 10.1029/2010GL043188
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 596SH
UT WOS:000277705200007
ER
PT J
AU Lopez, JJ
Greer, F
Greer, JR
AF Lopez, J. J.
Greer, F.
Greer, J. R.
TI Enhanced resistance of single-layer graphene to ion bombardment
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID AMORPHOUS-CARBON FILMS
AB We report that single-layer graphene on a SiO(2)/Si substrate withstands ion bombardment up to similar to 7 times longer than expected when exposed to focused Ga(+) ion beam. The exposure is performed in a dual beam scanning electron microscope/focused ion beam system at 30 kV accelerating voltage and 41 pA current. Ga(+) ion flux is determined by sputtering a known volume of hydrogenated amorphous carbon film deposited via plasma-enhanced chemical vapor deposition. (C) 2010 American Institute of Physics. [doi:10.1063/1.3428466]
C1 [Greer, J. R.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Lopez, J. J.] E Los Angeles Coll, Los Angeles, CA 91754 USA.
[Greer, F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Greer, JR (reprint author), CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
EM jrgreer@caltech.edu
RI Lopez, Josue/E-7508-2012
OI Lopez, Josue/0000-0001-8855-1330
FU NRI INDEX Center
FX We gratefully acknowledge financial support of the NRI INDEX Center. We
thank M. J. Burek for useful discussions and assistance with the
DualBeam system. Access to the Dual-Beam System was provided by the
Kavli Nanoscience Institute (KNI) at Caltech. We also appreciate
assistance from E. Miura and G. R. Rossman with Raman Spectroscopy, and
we thank C. Daraio for access to the optical microscope.
NR 22
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U1 0
U2 19
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 15
PY 2010
VL 107
IS 10
AR 104326
DI 10.1063/1.3428466
PG 4
WC Physics, Applied
SC Physics
GA 603BH
UT WOS:000278182400166
ER
PT J
AU Buzulukova, N
Fok, MC
Pulkkinen, A
Kuznetsova, M
Moore, TE
Glocer, A
Brandt, PC
Toth, G
Rastatter, L
AF Buzulukova, N.
Fok, M. -C.
Pulkkinen, A.
Kuznetsova, M.
Moore, T. E.
Glocer, A.
Brandt, P. C.
Toth, G.
Rastaetter, L.
TI Dynamics of ring current and electric fields in the inner magnetosphere
during disturbed periods: CRCM-BATS-R-US coupled model
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID RICE CONVECTION MODEL; NUMERICAL-SIMULATION; GEOMAGNETIC STORMS; ALIGNED
CURRENTS; MAGNETIC-FIELD; KINETIC-MODEL; PLASMA SHEET; SUBSTORM;
PRECIPITATION; ENERGY
AB We present simulation results from a one-way coupled global MHD model (Block-Adaptive-Tree Solar-Wind Roe-Type Upwind Scheme, BATS-R-US) and kinetic ring current models (Comprehensive Ring Current Model, CRCM, and Fok Ring Current, FokRC). The BATS-R-US provides the CRCM/FokRC with magnetic field information and plasma density/temperature at the polar CRCM/FokRC boundary. The CRCM uses an electric potential from the BATS-R-US ionospheric solver at the polar CRCM boundary in order to calculate the electric field pattern consistent with the CRCM pressure distribution. The FokRC electric field potential is taken from BATS-R-US ionospheric solver everywhere in the modeled region, and the effect of Region II currents is neglected. We show that for an idealized case with southward-northward-southward Bz IMF turning, CRCM-BATS-R-US reproduces well known features of inner magnetosphere electrodynamics: strong/weak convection under the southward/northward Bz; electric field shielding/overshielding/penetration effects; an injection during the substorm development; Subauroral Ion Drift or Polarization Jet (SAID/PJ) signature in the dusk sector. Furthermore, we find for the idealized case that SAID/PJ forms during the substorm growth phase, and that substorm injection has its own structure of field-aligned currents which resembles a substorm current wedge. For an actual event (12 August 2000 storm), we calculate ENA emissions and compare with Imager for Magnetopause-to-Aurora Global Exploration/High Energy Neutral Atom data. The CRCM-BATS-R-US reproduces both the global morphology of ring current and the fine structure of ring current injection. The FokRC-BATS-R-US shows the effect of a realistic description of Region II currents in ring current-MHD coupled models.
C1 [Buzulukova, N.; Fok, M. -C.; Pulkkinen, A.; Kuznetsova, M.; Moore, T. E.; Glocer, A.; Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pulkkinen, A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Brandt, P. C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Toth, G.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
RP Buzulukova, N (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 673,Bldg 21-261B,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM nbuzulukova@gmail.com
RI Glocer, Alex/C-9512-2012; Moore, Thomas/D-4675-2012; Rastaetter,
Lutz/D-4715-2012; Kuznetsova, Maria/F-6840-2012; Fok,
Mei-Ching/D-1626-2012; Toth, Gabor/B-7977-2013; feggans,
john/F-5370-2012; Brandt, Pontus/N-1218-2016
OI Glocer, Alex/0000-0001-9843-9094; Moore, Thomas/0000-0002-3150-1137;
Rastaetter, Lutz/0000-0002-7343-4147; Toth, Gabor/0000-0002-5654-9823;
Brandt, Pontus/0000-0002-4644-0306
FU NASA
FX This research was supported by NASA Science Mission Directorate,
Heliophysics Division, Heliophysics Guest Investigators Program, under
Work Breakdown Structure 955518. 02.01.02.57, and 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. The ACE SW and IMF data were obtained from the GSFC/SPDF
OMNIWeb interface at http://omniweb.gsfc.nasa.gov. The Dst, AU, AL, and
SYMH indices were provided from the WDC for Geomagnetism, Kyoto.
Simulation results for BATS-R-US and Ridley IE module have been provided
by the Community Coordinated Modeling Center at Goddard Space Flight
Center through their public Runs on Request System (
http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership
between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The BATS-R-US
model and Ridley IE solver were developed at Center for Space
Environment Modeling, University of Michigan. We are indebted to M.
Maddox for providing us with KAMELEON library. N. Buzulukova thanks A.
Dorodnitsyn for proofreading of the manuscript. The computer programs to
calculate ionospheric electrostatic potential in CRCM were written by S.
Sazykin. The authors thank A. Ridley for providing AMIE-derived CPCP.
NR 91
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U1 1
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY 15
PY 2010
VL 115
AR A05210
DI 10.1029/2009JA014621
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 596TO
UT WOS:000277708600003
ER
PT J
AU Hashmi, AJ
Eftekhar, AA
Adibi, A
Amoozegar, F
AF Hashmi, Ali Javed
Eftekhar, Ali Asghar
Adibi, Ali
Amoozegar, Farid
TI Analysis of telescope array receivers for deep-space inter-planetary
optical communication link between Earth and Mars
SO OPTICS COMMUNICATIONS
LA English
DT Article
DE Free space optical communication (FSO); Telescope array receiver;
Monte-Carlo simulations; Mars exploration
ID ATMOSPHERIC-TURBULENCE; PERFORMANCE
AB Optical communication technology shows promising prospects to fulfill the large bandwidth communication requirements of future deep-space exploration missions that are launched by NASA and various other international space agencies. At Earth, a telescope with a large aperture diameter is required to capture very weak optical signals that are transmitted from distant planets and to support large bandwidth communication link. A single large telescope has the limitations of cost, single point failure in case of malfunction, difficulty in manufacturing high quality optics, maintenance, and trouble in providing communication operations when transmitting spacecraft is close to the Sun. An array of relatively smaller-sized telescopes electrically connected to form an aggregate aperture area equivalent to a single large telescope is a viable alternative to a monolithic gigantic aperture. In this paper, we present the design concept and analysis of telescope array receivers for an optical communication link between Earth and Mars. Pulse-position modulation (PPM) is used at the transmitter end and photon-counting detectors along with the direct-detection technique are employed at each telescope element in the array. We also present the optimization of various system parameters, such as detector size (i.e., receiver field of view), PPM slot width, and the PPM order M, to mitigate the atmospheric turbulence and background noise effects, and to maximize the communication system performance. The performance of different array architectures is evaluated through analytical techniques and Monte-Carlo simulations for a broad range of operational scenarios, such as, Earth-Mars conjunction, Earth-Mars opposition, and different background and turbulence conditions. It is shown that the performance of the telescope array-based receiver is equivalent to a single large telescope; and as compared to current RF technology, telescope array-based optical receivers can provide several orders of magnitude greater data rates for deep-space communication with Mars. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Hashmi, Ali Javed; Eftekhar, Ali Asghar; Adibi, Ali] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Amoozegar, Farid] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Hashmi, AJ (reprint author), Georgia Inst Technol, 777 Atlantic Dr, Atlanta, GA 30332 USA.
EM hashmi@gatech.edu; Farid.Amoozegar@jpl.na-sa.gov
FU Jet Propulsion Laboratory (JPL), Pasadena, CA [NMO710820]
FX This work was performed at Georgia Institute of Technology and supported
by Jet Propulsion Laboratory (JPL), Pasadena, CA, under Contract Number
NMO710820.
NR 23
TC 10
Z9 11
U1 1
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0030-4018
J9 OPT COMMUN
JI Opt. Commun.
PD MAY 15
PY 2010
VL 283
IS 10
BP 2032
EP 2042
DI 10.1016/j.optcom.2010.01.073
PG 11
WC Optics
SC Optics
GA 585NQ
UT WOS:000276832900006
ER
PT J
AU Abadie, J
Abbott, BP
Abbott, R
Accadia, T
Acernese, F
Adhikari, R
Ajith, P
Allen, B
Allen, G
Ceron, EA
Amin, RS
Anderson, SB
Anderson, WG
Antonucci, F
Arain, MA
Araya, M
Arun, KG
Aso, Y
Aston, S
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Baker, P
Ballardin, G
Ballmer, S
Barker, D
Barone, F
Barr, B
Barriga, P
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Bauer, TS
Behnke, B
Beker, MG
Belletoile, A
Benacquista, M
Betzwieser, J
Beyersdorf, PT
Bigotta, S
Bilenko, IA
Billingsley, G
Birindelli, S
Biswas, R
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Blom, M
Boccara, C
Bock, O
Bodiya, TP
Bondarescu, R
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Bose, S
Bosi, L
Bouhou, B
Braccini, S
Bradaschia, C
Brady, PR
Braginsky, VB
Brau, JE
Breyer, J
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Budzynski, R
Bulik, T
Bullington, A
Bulten, HJ
Buonanno, A
Burmeister, O
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Cain, J
Calloni, E
Camp, JB
Campagna, E
Cannizzo, J
Cannon, KC
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Cardenas, L
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chalermsongsak, T
Chalkley, E
Charlton, P
Chassande-Mottin, E
Chatterji, S
Chelkowski, S
Chen, Y
Chincarini, A
Christensen, N
Chua, SSY
Chung, CTY
Clark, D
Clark, J
Clayton, JH
Cleva, F
Coccia, E
Colacino, CN
Colas, J
Colla, A
Colombini, M
Conte, R
Cook, D
Corbitt, TRC
Cornish, N
Corsi, A
Coulon, JP
Coward, D
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Culter, RM
Cumming, A
Cunningham, L
Cuoco, E
Dahl, K
Danilishin, SL
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Davier, M
Davies, G
Daw, EJ
Day, R
Dayanga, T
De Rosa, R
DeBra, D
Degallaix, J
del Prete, M
Dergachev, V
DeSalvo, R
Dhurandhar, S
Di Fiore, L
Di Lieto, A
Emilio, MD
Di Virgilio, A
Diaz, M
Dietz, A
Donovan, F
Dooley, KL
Doomes, EE
Drago, M
Drever, RWP
Driggers, J
Dueck, J
Duke, I
Dumas, JC
Edgar, M
Edwards, M
Effler, A
Ehrens, P
Etzel, T
Evans, M
Evans, T
Fafone, V
Fairhurst, S
Faltas, Y
Fan, Y
Fazi, D
Fehrmann, H
Ferrante, I
Fidecaro, F
Finn, LS
Fiori, I
Flaminio, R
Flasch, K
Foley, S
Forrest, C
Fotopoulos, N
Fournier, JD
Franc, J
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fulda, P
Fyffe, M
Galimberti, M
Gammaitoni, L
Garofoli, JA
Garufi, F
Gemme, G
Genin, E
Gennai, A
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Goetz, E
Goggin, LM
Gonzalez, G
Gossler, S
Gouaty, R
Granata, M
Grant, A
Gras, S
Gray, C
Greenhalgh, RJS
Gretarsson, AM
Greverie, C
Grosso, R
Grote, H
Grunewald, S
Guidi, GM
Gustafson, EK
Gustafson, R
Hage, B
Hallam, JM
Hammer, D
Hammond, GD
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Haughian, K
Hayama, K
Hayau, JF
Hayler, T
Heefner, J
Heitmann, H
Hello, P
Heng, IS
Heptonstall, A
Hewitson, M
Hild, S
Hirose, E
Hoak, D
Hodge, KA
Holt, K
Hosken, DJ
Hough, J
Howell, E
Hoyland, D
Huet, D
Hughey, B
Husa, S
Huttner, SH
Ingram, DR
Isogai, T
Ivanov, A
Jaranowski, P
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kandhasamy, S
Kanner, J
Katsavounidis, E
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Khalaidovski, A
Khalili, FY
Khan, R
Khazanov, E
Kim, H
King, PJ
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, R
Koranda, S
Kowalska, I
Kozak, D
Kringel, V
Krishnan, B
Krolak, A
Kuehn, G
Kullman, J
Kumar, R
Kwee, P
Lam, PK
Landry, M
Lang, M
Lantz, B
Lastzka, N
Lazzarini, A
Leaci, P
Lei, M
Leindecker, N
Leonor, I
Leroy, N
Letendre, N
Li, TGF
Lin, H
Lindquist, PE
Littenberg, TB
Lockerbie, NA
Lodhia, D
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Lu, P
Lubinski, M
Lucianetti, A
Luck, H
Lundgren, A
Machenschalk, B
MacInnis, M
Mageswaran, M
Mailand, K
Majorana, E
Mak, C
Maksimovic, I
Man, N
Mandel, I
Mandic, V
Mantovani, M
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Markowitz, J
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Marx, JN
Mason, K
Masserot, A
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McKechan, DJA
Mehmet, M
Melatos, A
Melissinos, AC
Mendell, G
Menendez, DF
Mercer, RA
Merill, L
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Milano, L
Miller, J
Minenkov, Y
Mino, Y
Mitra, S
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Mohan, M
Mohanty, SD
Mohapatra, SRP
Moreau, J
Moreno, G
Morgado, N
Morgia, A
Mors, K
Mosca, S
Moscatelli, V
Mossavi, K
Mours, B
MowLowry, C
Mueller, G
Mukherjee, S
Mullavey, A
Muller-Ebhardt, H
Munch, J
Murray, PG
Nash, T
Nawrodt, R
Nelson, J
Neri, I
Newton, G
Nishida, E
Nishizawa, A
Nocera, F
Ochsner, E
O'Dell, J
Ogin, GH
Oldenburg, R
O'Reilly, B
O'Shaughnessy, R
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Pagliaroli, G
Palladino, L
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Papa, MA
Pardi, S
Parisi, M
Pasqualetti, A
Passaquieti, R
Passuello, D
Patel, P
Pathak, D
Pedraza, M
Pekowsky, L
Penn, S
Peralta, C
Perreca, A
Persichetti, G
Pichot, M
Pickenpack, M
Piergiovanni, F
Pietka, M
Pinard, L
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Poggiani, R
Postiglione, F
Prato, M
Principe, M
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Raab, FJ
Rabeling, DS
Rabeling, DS
Radkins, H
Raffai, P
Raics, Z
Rakhmanov, M
Rapagnani, P
Raymond, V
Re, V
Reed, CM
Reed, T
Regimbau, T
Rehbein, H
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Roberts, P
Robertson, NA
Robinet, F
Robinson, C
Robinson, EL
Rocchi, A
Roddy, S
Rover, C
Rolland, L
Rollins, J
Romano, JD
Romano, R
Romie, JH
Rosinska, D
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Sakata, S
Salemi, F
Sammut, L
de la Jordana, LS
Sandberg, V
Sannibale, V
Santamaria, L
Santostasi, G
Saraf, S
Sarin, P
Sassolas, B
Sathyaprakash, BS
Sato, S
Satterthwaite, M
Saulson, PR
Savage, R
Schilling, R
Schnabel, R
Schofield, R
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Searle, AC
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sergeev, A
Shapiro, B
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Sintes, AM
Skelton, G
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, ND
Somiya, K
Sorazu, B
Sperandio, L
Stein, AJ
Stein, LC
Steplewski, S
Stochino, A
Stone, R
Strain, KA
Strigin, S
Stroeer, A
Sturani, R
Stuver, AL
Summerscales, TZ
Sung, M
Susmithan, S
Sutton, PJ
Swinkels, B
Szokoly, GP
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, JR
Taylor, R
Thorne, KA
Thorne, KS
Thuring, A
Titsler, C
Tokmakov, KV
Toncelli, A
Tonelli, M
Torres, C
Torrie, CI
Tournefier, E
Travasso, F
Traylor, G
Trias, M
Trummer, J
Turner, L
Ugolini, D
Urbanek, K
Vahlbruch, H
Vajente, G
Vallisneri, M
van den Brand, JFJ
Van Den Broeck, C
van der Putten, S
van der Sluys, MV
Vass, S
Vaulin, R
Vavoulidis, M
Vecchio, A
Vedovato, G
van Veggel, AA
Veitch, J
Veitch, PJ
Veltkamp, C
Verkindt, D
Vetrano, F
Vicere, A
Villar, A
Vinet, JY
Vocca, H
Vorvick, C
Vyachanin, SP
Waldman, SJ
Wallace, L
Wanner, A
Ward, RL
Was, M
Wei, P
Weinert, M
Weinstein, AJ
Weiss, R
Wen, L
Wen, S
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Wilmut, I
Winkelmann, L
Winkler, W
Wipf, CC
Wiseman, AG
Woan, G
Wooley, R
Worden, J
Yakushin, I
Yamamoto, H
Yamamoto, K
Yeaton-Massey, D
Yoshida, S
Yvert, M
Zanolin, M
Zhang, L
Zhang, Z
Zhao, C
Zotov, N
Zucker, ME
Zweizig, J
AF Abadie, J.
Abbott, B. P.
Abbott, R.
Accadia, T.
Acernese, F.
Adhikari, R.
Ajith, P.
Allen, B.
Allen, G.
Ceron, E. Amador
Amin, R. S.
Anderson, S. B.
Anderson, W. G.
Antonucci, F.
Arain, M. A.
Araya, M.
Arun, K. G.
Aso, Y.
Aston, S.
Astone, P.
Aufmuth, P.
Aulbert, C.
Babak, S.
Baker, P.
Ballardin, G.
Ballmer, S.
Barker, D.
Barone, F.
Barr, B.
Barriga, P.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Bastarrika, M.
Bauer, Th. S.
Behnke, B.
Beker, M. G.
Belletoile, A.
Benacquista, M.
Betzwieser, J.
Beyersdorf, P. T.
Bigotta, S.
Bilenko, I. A.
Billingsley, G.
Birindelli, S.
Biswas, R.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Bland, B.
Blom, M.
Boccara, C.
Bock, O.
Bodiya, T. P.
Bondarescu, R.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Bose, S.
Bosi, L.
Bouhou, B.
Braccini, S.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Brau, J. E.
Breyer, J.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Budzynski, R.
Bulik, T.
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Sancho de la Jordana, L.
Sandberg, V.
Sannibale, V.
Santamaria, L.
Santostasi, G.
Saraf, S.
Sarin, P.
Sassolas, B.
Sathyaprakash, B. S.
Sato, S.
Satterthwaite, M.
Saulson, P. R.
Savage, R.
Schilling, R.
Schnabel, R.
Schofield, R.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Searle, A. C.
Seifert, F.
Sellers, D.
Sengupta, A. S.
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Sergeev, A.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
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Sintes, A. M.
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Slagmolen, B. J. J.
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Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, H. R.
Williams, L.
Willke, B.
Wilmut, I.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Woan, G.
Wooley, R.
Worden, J.
Yakushin, I.
Yamamoto, H.
Yamamoto, K.
Yeaton-Massey, D.
Yoshida, S.
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Zanolin, M.
Zhang, L.
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Zweizig, J.
CA LIGO Sci Collaboration
Virgo Collaboration
TI All-sky search for gravitational-wave bursts in the first joint
LIGO-GEO-Virgo run
SO PHYSICAL REVIEW D
LA English
DT Article
ID PERFORMANCE
AB We present results from an all-sky search for unmodeled gravitational-wave bursts in the data collected by the LIGO, GEO 600 and Virgo detectors between November 2006 and October 2007. The search is performed by three different analysis algorithms over the frequency band 50-6000 Hz. Data are analyzed for times with at least two of the four LIGO-Virgo detectors in coincident operation, with a total live time of 266 days. No events produced by the search algorithms survive the selection cuts. We set a frequentist upper limit on the rate of gravitational-wave bursts impinging on our network of detectors. When combined with the previous LIGO search of the data collected between November 2005 and November 2006, the upper limit on the rate of detectable gravitational-wave bursts in the 64-2048 Hz band is 2.0 events per year at 90% confidence. We also present event rate versus strength exclusion plots for several types of plausible burst waveforms. The sensitivity of the combined search is expressed in terms of the root-sum-squared strain amplitude for a variety of simulated waveforms and lies in the range 6 x 10(-22) Hz(-1/2) to 2 x 10(-20) Hz(-1/2). This is the first untriggered burst search to use data from the LIGO and Virgo detectors together, and the most sensitive untriggered burst search performed so far.
C1 [Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Anderson, S. B.; Araya, M.; Aso, Y.; Ballmer, S.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cannon, K. C.; Cardenas, L.; Cepeda, C.; Chalermsongsak, T.; Chatterji, S.; Coyne, D. C.; Daudert, B.; DeSalvo, R.; Driggers, J.; Ehrens, P.; Etzel, T.; Fazi, D.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A.; Hodge, K. A.; Ivanov, A.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Kozak, D.; Lazzarini, A.; Lei, M.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Mak, C.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Mitra, S.; Miyakawa, O.; Nash, T.; Ogin, G. H.; Patel, P.; Pedraza, M.; Robertson, N. A.; Sannibale, V.; Searle, A. C.; Seifert, F.; Sengupta, A. S.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Turner, L.; Vass, S.; Villar, A.; Wallace, L.; Ward, R. L.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Papa, M. A.; Peralta, C.; Robinson, E. L.; Santamaria, L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Allen, B.; Aulbert, C.; Bock, O.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; Dueck, J.; Fehrmann, H.; Frede, M.; Friedrich, D.; Giampanis, S.; Gossler, S.; Grote, H.; Hayama, K.; Hewitson, M.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kullman, J.; Lastzka, N.; Leaci, P.; Lueck, H.; Machenschalk, B.; Mehmet, M.; Messenger, C.; Mors, K.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Prix, R.; Puncken, O.; Rehbein, H.; Roever, C.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schulz, B.; Seifert, F.; Taylor, J. R.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Willke, B.; Winkelmann, L.; Winkler, W.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Roberts, P.; Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Barsuglia, M.; Bouhou, B.; Buy, C.; Chassande-Mottin, E.; Granata, M.] Univ Paris 07, CEA, Observ Paris, APC,CNRS,UMR7164,IN2P3,DSM,IRFU, F-75221 Paris 05, France.
[Chua, S. S. Y.; Lam, P. K.; McClelland, D. E.; MowLowry, C.; Mullavey, A.; Rabeling, D. S.; Satterthwaite, M.; Scott, S. M.; Slagmolen, B. J. J.; Wette, K.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Chen, Y.; Mino, Y.; Somiya, K.; Thorne, K. S.; Vallisneri, M.; Wen, L.] CALTECH CaRT, Pasadena, CA 91125 USA.
[Clark, J.; Davies, G.; Edwards, M.; Fairhurst, S.; Harry, I. W.; Jones, G.; McKechan, D. J. A.; Pathak, D.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Van Den Broeck, C.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Christensen, N.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
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RP Abadie, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Khan, Rubab/F-9455-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Postiglione, Fabio/O-4744-2015; Rocchi,
Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; mosca,
simona/I-7116-2012; Frasconi, Franco/K-1068-2016; Sigg,
Daniel/I-4308-2015; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Ferrante, Isidoro/F-1017-2012; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Pitkin,
Matthew/I-3802-2013; Vyatchanin, Sergey/J-2238-2012; Miao,
Haixing/O-1300-2013; Khazanov, Efim/B-6643-2014; Salemi,
Francesco/F-6988-2014; Lucianetti, Antonio/G-7383-2014; Losurdo,
Giovanni/K-1241-2014; Lam, Ping Koy/A-5276-2008; Danilishin,
Stefan/K-7262-2012; Canuel, Benjamin/C-7459-2014; Khalili,
Farit/D-8113-2012; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Mitrofanov, Valery/D-8501-2012; Puppo,
Paola/J-4250-2012; Rapagnani, Piero/J-4783-2012; Gemme,
Gianluca/C-7233-2008; 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; Parisi,
Maria/D-2817-2013; Colla, Alberto/J-4694-2012; Drago, Marco/E-7134-2013;
Re, Virginia /F-6403-2013; Vocca, Helios/F-1444-2010; Acernese,
Fausto/E-4989-2010; Finn, Lee Samuel/A-3452-2009; Hammond,
Giles/B-7861-2009; Prato, Mirko/D-8531-2012; prodi,
giovanni/B-4398-2010; Rowan, Sheila/E-3032-2010; McClelland,
David/E-6765-2010; Prokhorov, Leonid/I-2953-2012; Punturo,
Michele/I-3995-2012; Strigin, Sergey/I-8337-2012; Cuoco,
Elena/I-8789-2012; Vicere, Andrea/J-1742-2012; Strain,
Kenneth/D-5236-2011; Gammaitoni, Luca/B-5375-2009; Neri,
Igor/F-1482-2010; Hild, Stefan/A-3864-2010; Martin, Iain/A-2445-2010;
Lueck, Harald/F-7100-2011; Kawazoe, Fumiko/F-7700-2011; Bigotta,
Stefano/F-8652-2011; Freise, Andreas/F-8892-2011; Marchesoni,
Fabio/A-1920-2008; Kawabe, Keita/G-9840-2011; Bondu,
Francois/A-2071-2012; Toncelli, Alessandra/A-5352-2012; Hammond,
Giles/A-8168-2012; Howell, Eric/H-5072-2014; Cella,
Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Frey,
Raymond/E-2830-2016; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Ward, Robert/I-8032-2014;
OI Khan, Rubab/0000-0001-5100-5168; Garufi, Fabio/0000-0003-1391-6168;
Postiglione, Fabio/0000-0003-0628-3796; Rocchi,
Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616;
mosca, simona/0000-0001-7869-8275; Frasconi, Franco/0000-0003-4204-6587;
Sigg, Daniel/0000-0003-4606-6526; Ferrante, Isidoro/0000-0002-0083-7228;
Travasso, Flavio/0000-0002-4653-6156; Pitkin,
Matthew/0000-0003-4548-526X; Miao, Haixing/0000-0003-4101-9958; Losurdo,
Giovanni/0000-0003-0452-746X; Lam, Ping Koy/0000-0002-4421-601X;
Danilishin, Stefan/0000-0001-7758-7493; Vecchio,
Alberto/0000-0002-6254-1617; Puppo, Paola/0000-0003-4677-5015; Gemme,
Gianluca/0000-0002-1127-7406; Allen, Bruce/0000-0003-4285-6256; Zhao,
Chunnong/0000-0001-5825-2401; Vocca, Helios/0000-0002-1200-3917;
Acernese, Fausto/0000-0003-3103-3473; Finn, Lee
Samuel/0000-0002-3937-0688; Prato, Mirko/0000-0002-2188-8059; prodi,
giovanni/0000-0001-5256-915X; McClelland, David/0000-0001-6210-5842;
Punturo, Michele/0000-0001-8722-4485; Vicere,
Andrea/0000-0003-0624-6231; Strain, Kenneth/0000-0002-2066-5355;
Gammaitoni, Luca/0000-0002-4972-7062; Neri, Igor/0000-0002-9047-9822;
Lueck, Harald/0000-0001-9350-4846; Marchesoni,
Fabio/0000-0001-9240-6793; Bondu, Francois/0000-0001-6487-5197;
Toncelli, Alessandra/0000-0003-4400-8808; Aulbert,
Carsten/0000-0002-1481-8319; Di Paolo Emilio,
Maurizio/0000-0002-9558-3610; PERSICHETTI, GIANLUCA/0000-0001-8424-9791;
Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946;
Whiting, Bernard F/0000-0002-8501-8669; Veitch,
John/0000-0002-6508-0713; Zweizig, John/0000-0002-1521-3397;
O'Shaughnessy, Richard/0000-0001-5832-8517; Pathak,
Devanka/0000-0002-1768-8353; Granata, Massimo/0000-0003-3275-1186;
Santamaria, Lucia/0000-0002-5986-0449; Coccia,
Eugenio/0000-0002-6669-5787; Hallam, Jonathan Mark/0000-0002-7087-0461;
Vetrano, Flavio/0000-0002-7523-4296; Nishizawa,
Atsushi/0000-0003-3562-0990; calloni, enrico/0000-0003-4819-3297;
Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
Vedovato, Gabriele/0000-0001-7226-1320; Howell,
Eric/0000-0001-7891-2817; Fairhurst, Stephen/0000-0001-8480-1961;
Matichard, Fabrice/0000-0001-8982-8418; Husa,
Sascha/0000-0002-0445-1971; Pinto, Innocenzo M./0000-0002-2679-4457;
Guidi, Gianluca/0000-0002-3061-9870; Cella,
Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167;
Frey, Raymond/0000-0003-0341-2636; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Jaranowski, Piotr/0000-0001-8085-3414;
Stein, Leo/0000-0001-7559-9597; Swinkels, Bas/0000-0002-3066-3601; Ward,
Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan,
John/0000-0001-5710-6576; Principe, Maria/0000-0002-6327-0628; Papa,
M.Alessandra/0000-0002-1007-5298; Kanner, Jonah/0000-0001-8115-0577
FU 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; Foundation for
Fundamental Research on Matter; Netherlands Organisation for Scientific
Research; Polish Ministry of Science and Higher Education; Foundation
for Polish Science; Royal Society; Scottish Funding Council; Scottish
Universities Physics Alliance; National Aeronautics and Space
Administration; Carnegie Trust; Leverhulme Trust; David and Lucile
Packard Foundation; Research Corporation; Alfred P. Sloan Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society and the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO 600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo 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
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, the Polish Ministry of
Science and Higher Education, the FOCUS Programme of Foundation for
Polish Science, 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. This document has been assigned LIGO
Laboratory document number LIGO-P0900108-v6.
NR 39
TC 36
Z9 36
U1 1
U2 23
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 15
PY 2010
VL 81
IS 10
AR 102001
DI 10.1103/PhysRevD.81.102001
PG 20
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 602NS
UT WOS:000278146700004
ER
PT J
AU Foster, G
Annan, JD
Jones, PD
Mann, ME
Mullan, B
Renwick, J
Salinger, J
Schmidt, GA
Trenberth, KE
AF Foster, G.
Annan, J. D.
Jones, P. D.
Mann, M. E.
Mullan, B.
Renwick, J.
Salinger, J.
Schmidt, G. A.
Trenberth, K. E.
TI Comment on "Influence of the Southern Oscillation on tropospheric
temperature" by J. D. McLean, C. R. de Freitas, and R. M. Carter
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SURFACE-TEMPERATURE; VOLCANOS; ENSO
AB McLean et al. (2009) (henceforth MFC09) claim that the El Nino-Southern Oscillation (ENSO), as represented by the Southern Oscillation Index (SOI), accounts for as much as 72% of the global tropospheric temperature anomaly and an even higher 81% of this anomaly in the tropics. They conclude that the SOI is a "dominant and consistent influence on mean global temperatures," "and perhaps recent trends in global temperatures." However, their analysis is inappropriate in a number of ways and overstates the influence of ENSO on the climate system. This comment first briefly reviews what is understood about the influence of ENSO on global temperatures and then shows that the analysis of MFC09 greatly overestimates the correlation between temperature anomalies and the SOI by inflating the power in the 2-6 year time window while filtering out variability on longer and shorter time scales. The suggestion in their conclusions that ENSO may be a major contributor to recent trends in global temperature is not supported by their analysis or any physical theory presented in their paper, especially as the analysis method itself eliminates the influence of trends on the purported correlations.
C1 [Foster, G.] Tempo Analyt, Westbrook, ME 04092 USA.
[Annan, J. D.] JAMSTEC, Res Inst Global Change, Kanazawa Ku, Kanagawa 2360001, Japan.
[Jones, P. D.] Univ E Anglia, Sch Environm Sci, Climat Res Unit, Norwich NR4 7TJ, Norfolk, England.
[Mann, M. E.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Mullan, B.; Renwick, J.] NIWA, Climate Variabil Grp, Wellington 6241, New Zealand.
[Salinger, J.] Univ Auckland, Sch Environm, Auckland 1142, New Zealand.
[Schmidt, G. A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Trenberth, K. E.] NCAR, Climate Anal Sect, Boulder, CO 80307 USA.
[Mann, M. E.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA.
RP Foster, G (reprint author), Tempo Analyt, 146C Mech St, Westbrook, ME 04092 USA.
EM jdannan@jamstec.go.jp
RI Jones, Philip/C-8718-2009; Trenberth, Kevin/A-5683-2012; Schmidt,
Gavin/D-4427-2012; Annan, James/A-3702-2010; Mann, Michael/B-8472-2017
OI Jones, Philip/0000-0001-5032-5493; Trenberth, Kevin/0000-0002-1445-1000;
Schmidt, Gavin/0000-0002-2258-0486; Mann, Michael/0000-0003-3067-296X
FU Ministry of the Environment, Japan [S-5-1]; National Science Foundation;
U.S. Department Of Energy [DE-FG02-98ER62601]
FX This work was supported by the Global Environment Research Fund (S-5-1)
of the Ministry of the Environment, Japan. NCAR is supported by the
National Science Foundation. P.D.J. has been supported by the U.S.
Department Of Energy (grant DE-FG02-98ER62601). We are grateful to three
reviewers for useful comments.
NR 10
TC 4
Z9 4
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 MAY 14
PY 2010
VL 115
AR D09110
DI 10.1029/2009JD012960
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 596SP
UT WOS:000277706000004
ER
PT J
AU Stano, GT
Fuelberg, HE
Roeder, WP
AF Stano, Geoffrey T.
Fuelberg, Henry E.
Roeder, William P.
TI Developing empirical lightning cessation forecast guidance for the Cape
Canaveral Air Force Station and Kennedy Space Center
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID UNITED-STATES; DETECTION NETWORK; FLORIDA; ELECTRIFICATION;
THUNDERSTORMS; CLIMATOLOGY; PARAMETERS; MECHANISM; UPDRAFT; RATES
AB This research addresses the 45th Weather Squadron's (45WS) need for improved guidance regarding lightning cessation at Cape Canaveral Air Force Station and Kennedy Space Center (KSC). KSC's Lightning Detection and Ranging (LDAR) network was the primary observational tool to investigate both cloud-to-ground and intracloud lightning. Five statistical and empirical schemes were created from LDAR, sounding, and radar parameters derived from 116 storms. Four of the five schemes were unsuitable for operational use since lightning advisories would be canceled prematurely, leading to safety risks to personnel. These include a correlation and regression tree analysis, three variants of multiple linear regression, event time trending, and the time delay between the greatest height of the maximum dBZ value to the last flash. These schemes failed to adequately forecast the maximum interval, the greatest time between any two flashes in the storm. The majority of storms had a maximum interval less than 10 min, which biased the schemes toward small values. Success was achieved with the percentile method (PM) by separating the maximum interval into percentiles for the 100 dependent storms. PM provides additional confidence to the 45WS forecasters, and a modified version was incorporated into their forecast procedures starting in the summer of 2008. This inclusion has resulted in similar to 5-10 min time savings. Last, an experimental regression variant scheme using non-real-time predictors produced precise results but prematurely ended advisories. This precision suggests that obtaining these parameters in real time may provide useful added information to the PM scheme.
C1 [Stano, Geoffrey T.; Fuelberg, Henry E.] Florida State Univ, Dept Meteorol, Tallahassee, FL 32306 USA.
RP Fuelberg, HE (reprint author), NASA, NASA Short Term Predict Res & Transit Program, 320 Sparkman Dr, Huntsville, AL 35812 USA.
EM geoffrey.stano@nasa.gov; fuelberg@met.fsu.edu;
william.roeder@patrick.af.mil
FU NASA [NNK06EB17G]
FX Special thanks go to Todd McNamara of the 45th Weather Squadron for his
help with several technical aspects of this research, along with his
operational knowledge. We also thank Lee Nelson for the use of his flash
creation algorithm. Additional thanks goes to the numerous individuals
who provided critiques and suggestions for improving this work at the
1st International Lightning Meteorology Conference (ILMC) in Tucson,
Arizona, in 2006. This research was sponsored by NASA's Innovative
Partner's Program under grant NNK06EB17G.
NR 74
TC 6
Z9 6
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 MAY 14
PY 2010
VL 115
AR D09205
DI 10.1029/2009JD013034
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 596SP
UT WOS:000277706000005
ER
PT J
AU Holstein-Rathlou, C
Gunnlaugsson, HP
Merrison, JP
Bean, KM
Cantor, BA
Davis, JA
Davy, R
Drake, NB
Ellehoj, MD
Goetz, W
Hviid, SF
Lange, CF
Larsen, SE
Lemmon, MT
Madsen, MB
Malin, M
Moores, JE
Nornberg, P
Smith, P
Tamppari, LK
Taylor, PA
AF Holstein-Rathlou, C.
Gunnlaugsson, H. P.
Merrison, J. P.
Bean, K. M.
Cantor, B. A.
Davis, J. A.
Davy, R.
Drake, N. B.
Ellehoj, M. D.
Goetz, W.
Hviid, S. F.
Lange, C. F.
Larsen, S. E.
Lemmon, M. T.
Madsen, M. B.
Malin, M.
Moores, J. E.
Nornberg, P.
Smith, P.
Tamppari, L. K.
Taylor, P. A.
TI Winds at the Phoenix landing site
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MARS-COLOR-IMAGER; MARTIAN ATMOSPHERE; ORBITER; SURFACE; CLIMATE; LAYER
AB Wind speeds and directions were measured on the Phoenix Lander by a mechanical anemometer, the so-called Telltale wind indicator. Analysis of images of the instrument taken with the onboard imager allowed for evaluation of wind speeds and directions. Daily characteristics of the wind data are highly turbulent behavior during midday due to daytime turbulence with more stable conditions during nighttime. From L(s)similar to 77 degrees-123 degrees winds were generally similar to 4 m s(-1) from the east, with 360 degrees rotation during midday. From L(s) similar to 123 degrees-148 degrees daytime wind speeds increased to an average of 6-10 m s(-1) and were generally from the west. The highest wind speed recorded was 16 m s(-1) seen on L(s) similar to 147 degrees. Estimates of the surface roughness height are calculated from the smearing of the Kapton part of the Telltale during image exposure due to a 3 Hz turbulence and nighttime wind variability. These estimates yield 6 +/- 3 mm and 5 +/- 3 mm, respectively. The Telltale wind data are used to suggest that Heimdal crater is a source of nighttime temperature fluctuations. Deviations between temperatures measured at various heights are explained as being due to winds passing over the Phoenix Lander. Events concerning sample delivery and frost formation are described and discussed. Two different mechanisms of dust lifting affecting the Phoenix site are proposed based on observations made with Mars Color Imager on Mars Reconnaissance Orbiter and the Telltale. The first is related to evaporation of the seasonal CO(2) ice and is observed up to L(s) similar to 95 degrees. These events are not associated with increased wind speeds. The second mechanism is observed after L(s) similar to 111 degrees and is related to the passing of weather systems characterized by condensate clouds in orbital images and higher wind speeds as measured with the Telltale.
C1 [Holstein-Rathlou, C.; Gunnlaugsson, H. P.; Merrison, J. P.; Nornberg, P.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Bean, K. M.; Lemmon, M. T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Cantor, B. A.; Malin, M.] Malin Space Sci Syst Inc, San Diego, CA 92191 USA.
[Davis, J. A.; Lange, C. F.] Univ Alberta, Dept Mech Engn, Edmonton, AB T6G 2M7, Canada.
[Davy, R.; Taylor, P. A.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Drake, N. B.] DE Shaw Res, New York, NY 10036 USA.
[Ellehoj, M. D.; Madsen, M. B.] Univ Copenhagen, Niels Bohr Inst, DK-1165 Copenhagen, Denmark.
[Goetz, W.; Hviid, S. F.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Larsen, S. E.] Tech Univ Denmark, Risoe Natl Lab, Wind Energy Dept, DK-4000 Roskilde, Denmark.
[Moores, J. E.; Smith, P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85719 USA.
[Tamppari, L. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Holstein-Rathlou, C (reprint author), Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
EM holstein@phys.au.dk
RI Nornberg, Per/A-6228-2012; Lemmon, Mark/E-9983-2010; Madsen,
Morten/D-2082-2011; Davy, Richard/H-8387-2016;
OI Lemmon, Mark/0000-0002-4504-5136; Madsen, Morten/0000-0001-8909-5111;
Davy, Richard/0000-0001-9639-5980; Ellehoj, Mads/0000-0002-6961-2537;
merrison, jonathan/0000-0003-4362-6356
FU Danish Natural Science Research Council; Canadian Space Agency
FX The Telltale project has been supported by the Danish Natural Science
Research Council. The support of the Canadian Space Agency for the work
of J. A. Davis and C. F. Lange is gratefully acknowledged. The authors
acknowledge A. Leung for CFD simulations of the Telltale, and J. Boddez
and G. Heacock for creation of the Open Lander model used in the CFD
simulations. L. Tamppari's contribution to the research described in
this paper was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA.
NR 39
TC 36
Z9 36
U1 0
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY 14
PY 2010
VL 115
AR E00E18
DI 10.1029/2009JE003411
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 596TD
UT WOS:000277707500001
ER
PT J
AU Tamppari, LK
Bass, D
Cantor, B
Daubar, I
Dickinson, C
Fisher, D
Fujii, K
Gunnlauggson, HP
Hudson, TL
Kass, D
Kleinbohl, A
Komguem, L
Lemmon, MT
Mellon, M
Moores, J
Pankine, A
Pathak, J
Searls, M
Seelos, F
Smith, MD
Smrekar, S
Taylor, P
Holstein-Rathlou, C
Weng, WS
Whiteway, J
Wolff, M
AF Tamppari, Leslie K.
Bass, Deborah
Cantor, Bruce
Daubar, Ingrid
Dickinson, Cameron
Fisher, David
Fujii, Ken
Gunnlauggson, Haraldur P.
Hudson, Troy L.
Kass, David
Kleinboehl, Armin
Komguem, Leonce
Lemmon, Mark T.
Mellon, Mike
Moores, John
Pankine, Alexey
Pathak, Jagruti
Searls, Mindi
Seelos, Frank
Smith, Michael D.
Smrekar, Sue
Taylor, Peter
Holstein-Rathlou, Christina
Weng, Wensong
Whiteway, Jim
Wolff, Mike
TI Phoenix and MRO coordinated atmospheric measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; WATER-ICE CLOUDS; ORBITER CAMERA OBSERVATIONS;
MARTIAN DUST STORMS; NORTH POLAR-REGION; MARS-COLOR-IMAGER; MGS TES;
INTERANNUAL VARIABILITY; VERTICAL DISTRIBUTION; VAPOR
AB The Phoenix and Mars Reconnaissance Orbiter (MRO) missions collaborated in an unprecedented campaign to observe the northern polar region summer atmosphere throughout the Phoenix mission (25 May to 2 November 2008; L-s = 76 degrees-150 degrees) and slightly beyond (similar to L-s = 158 degrees). Five atmospherically related campaigns were defined a priori and were executed on 37 separate Martian days (sols). Phoenix and MRO observed the atmosphere nearly simultaneously. We describe the observation strategy and history, the participating experiments, and some initial results. We find that there is general agreement between measurements from different instruments and platforms and that complementary measurements provide a consistent picture of the atmosphere. Seasonal water abundance behavior matches with historical measurements. Winds aloft, as measured by cloud motions, showed the same seasonally consistent, diurnal rotation as the winds measured at the lander, during the first part of the mission (L-s = 76 degrees-118 degrees). A diurnal cycle recorded from L-s similar to 108.3 degrees-109.1 degrees, in which a dust front was approaching the Phoenix Lander, is examined in detail. Cloud heights measured on subsequent orbits showed that in areas of active lifting, dust can be lofted quite high in the atmosphere, doubling in height over 2 h. The combination of experiments also revealed that there were discrete vertical layers of water ice and dust. Water vapor column abundances compared to near-surface water vapor pressure indicate that water is not well mixed from the surface to a cloud condensation height and that the depth of the layer that exchanges diurnally with the surface is 0.5-1 km.
C1 [Tamppari, Leslie K.; Bass, Deborah; Fujii, Ken; Hudson, Troy L.; Kass, David; Kleinboehl, Armin; Pankine, Alexey; Smrekar, Sue] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cantor, Bruce] Malin Space Sci Syst Inc, San Diego, CA 92121 USA.
[Daubar, Ingrid; Moores, John] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Dickinson, Cameron; Komguem, Leonce; Pathak, Jagruti; Taylor, Peter; Weng, Wensong; Whiteway, Jim] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 1P3, Canada.
[Fisher, David] Geol Survey Canada, Ottawa, ON K1A 0E4, Canada.
[Gunnlauggson, Haraldur P.; Holstein-Rathlou, Christina] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark.
[Lemmon, Mark T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Mellon, Mike; Searls, Mindi] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Seelos, Frank] Johns Hopkins Univ, APL, Laurel, MD 20723 USA.
[Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Whiteway, Jim] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Wolff, Mike] Space Sci Inst, Boulder, CO 80301 USA.
RP Tamppari, LK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM leslie.tamppari@jpl.nasa.gov
RI Smith, Michael/C-8875-2012; Lemmon, Mark/E-9983-2010; Daubar,
Ingrid/N-1408-2013; Mellon, Michael/C-3456-2016; Seelos,
Frank/C-7875-2016
OI Lemmon, Mark/0000-0002-4504-5136; Seelos, Frank/0000-0001-9721-941X
NR 73
TC 24
Z9 24
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY 14
PY 2010
VL 115
AR E00E17
DI 10.1029/2009JE003415
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 596TD
UT WOS:000277707500002
ER
PT J
AU Burchill, JK
Knudsen, DJ
Clemmons, JH
Oksavik, K
Pfaff, RF
Steigies, CT
Yau, AW
Yeoman, TK
AF Burchill, J. K.
Knudsen, D. J.
Clemmons, J. H.
Oksavik, K.
Pfaff, R. F.
Steigies, C. T.
Yau, A. W.
Yeoman, T. K.
TI Thermal ion upflow in the cusp ionosphere and its dependence on soft
electron energy flux
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID LATITUDE F-REGION; MASS-SPECTROMETER OBSERVATIONS; POLAR WIND;
MAGNETOSPHERIC PLASMA; EISCAT OBSERVATIONS; AURORAL ACTIVITY; OUTFLOW;
ALTITUDE; ACCELERATION; ENERGIZATION
AB We investigate the origin of low-energy (E-k < 10 eV) ion upflows in Earth's low-altitude dayside cusp region. The Cusp-2002 sounding rocket flew from Ny Alesund, Svalbard, on 14 December 2002, carrying plasma and field instrumentation to an altitude of 768 km. The Suprathermal Ion Imager, a two-dimensional energy/arrival angle spectrograph, observed large (> 500 m s(-1)) ion upflows within the cusp at altitudes between 640 km and 768 km. We report a significant correlation between ion upflow and precipitating magnetosheath electron energy flux in this altitude range. There is only very weak correlation between upflow and wave power in the VLF band. We find a small negative correlation between upflow and the magnitude of the DC electric field for fields less than about 70 mV m(-1). The apparent relation between upflow and electron energy flux suggests a mechanism whereby ions are accelerated by parallel electric fields that are established by the soft electrons. Significant ion upflows are not observed for electron energy fluxes less than about 10(10) eV cm(-2) s(-1). The lack of correspondence between |(E) over right arrow| and upflow on the one hand, and wave power and upflow on the other, does not rule out these processes but implies that, if operating, they are not local to the measurement region. We also observe narrow regions of large ion downflow that imply either a rebalancing of the ionosphere toward a low-T-e equilibrium during which gravity dominates over the pressure gradients or a convection of the upflowing ions away from the precipitation region, outside of which the ions must fall back into equilibrium at lower altitudes.
C1 [Burchill, J. K.; Knudsen, D. J.; Yau, A. W.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Clemmons, J. H.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90245 USA.
[Oksavik, K.] Univ Ctr Svalbard, Dept Arctic Geophys, N-9171 Longyearbyen, Norway.
[Pfaff, R. F.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Steigies, C. T.] Univ Kiel, Inst Expt & Angew Phys, D-24098 Kiel, Germany.
[Yeoman, T. K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Burchill, JK (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM burchill@phys.ucalgary.ca
RI Pfaff, Robert/F-5703-2012; Yau, Andrew/E-7007-2013; Yeoman,
Timothy/L-9105-2014;
OI Pfaff, Robert/0000-0002-4881-9715; Yau, Andrew/0000-0002-8210-0392;
Yeoman, Timothy/0000-0002-8434-4825; Oksavik,
Kjellmar/0000-0003-4312-6992
FU Canadian Space Agency; Natural Sciences and Engineering Research Council
of Canada; NASA [NAG5-5264]
FX This research was supported by the Canadian Space Agency and the Natural
Sciences and Engineering Research Council of Canada. The Cusp SII
development was supported by a contract from the Canadian Space Agency.
The Aerospace Corporation acknowledges NASA support through grant
NAG5-5264. The authors acknowledge the contributions and expertise of
the SII development team (K. Berg, G. Enno, P. King, C. Marcellus, and
I. Wevers) at the Institute for Space Research of the University of
Calgary. We would like to thank the PIs of the Northern Hemisphere
SuperDARN radars (W. A. Bristow, R. A. Greenwald, T. Kikuchi, M. Lester,
M. Pinnock, G. Sofko, and J.-P. Villain) for providing SuperDARN data
for this interval. CUSTLASS is a PPARC UK National Facility operated by
the University of Leicester. EISCAT is an international scientific
association supported by research organizations of China (CRIRP),
Finland (SA), France (CNRS, till the end of 2006), Germany (DFG), Japan
(NIPR and STEL), Norway (NFR), Sweden (VR), and the United Kingdom
(STFC). J.K.B. appreciates helpful discussions on the ion upflow
measurements with W. Peterson, J.-P. St. Maurice, L. Kagan, S. Buchert,
B. Jackel, and P. Amerl.
NR 58
TC 15
Z9 15
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY 14
PY 2010
VL 115
AR A05206
DI 10.1029/2009JA015006
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 596TN
UT WOS:000277708500003
ER
PT J
AU Samsonov, AA
Sibeck, DG
Yu, YQ
AF Samsonov, A. A.
Sibeck, D. G.
Yu, Yiqun
TI Transient changes in magnetospheric-ionospheric currents caused by the
passage of an interplanetary shock: Northward interplanetary magnetic
field case
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GEOMAGNETIC SUDDEN COMMENCEMENT; 3-DIMENSIONAL MHD SIMULATION; LATITUDE
BOUNDARY-LAYER; NUMERICAL-SIMULATION; BIRKELAND CURRENTS; ALIGNED
CURRENTS; CURRENT SYSTEMS; IMF CONDITIONS; CONVECTION; IMPULSE
AB We use results from a global MHD simulation to study the interaction of an interplanetary shock with the Earth's magnetosphere for a northward interplanetary magnetic field orientation. We connect intensifications of the transient northward Bz (NBZ) and Region 1 currents in the ionosphere with the appearance of two strong dynamo regions in the magnetosphere: the first on the high-latitude magnetopause near and behind the cusps and the second near the equatorial plane on the flanks. The ionospheric and magnetospheric transients are well synchronized and move antisunward gradually. According to the results obtained, the source of energy for the transient NBZ current is related to shock-intensified lobe reconnection, while the transient Region 1 current corresponds to the reflected fast shock predicted by Samsonov et al. (2007). We speculate that the electric circuits for the quasi-stationary field-aligned currents are similar to the transient electric circuits obtained in this paper.
C1 [Samsonov, A. A.] St Petersburg State Univ, Dept Earth Phys, St Petersburg 198504, Russia.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yu, Yiqun] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Samsonov, AA (reprint author), St Petersburg State Univ, Dept Earth Phys, St Petersburg 198504, Russia.
EM samsonov@geo.phys.spbu.ru
RI Sibeck, David/D-4424-2012; Samsonov, Andrey/I-7057-2012; Yu,
Yiqun/E-2710-2012
OI Samsonov, Andrey/0000-0001-8243-1151; Yu, Yiqun/0000-0002-1013-6505
FU NASA; Russian President [NSH-1243.2008.5]; GK [N 02.740.11.0331]
FX The work was supported in part by NASA's THEMIS project and in part by
grant of Russian President NSH-1243.2008.5 and GK grant N
02.740.11.0331. Simulation results have been provided by the Community
Coordinated Modeling Center (CCMC) at Goddard Space Flight Center
through their public Runs on Request system (http://ccmc.gsfc.nasa.gov).
In particular, we have studied the run "Andrey_Samsonov_120507_1." The
BATS-R-US Model was developed by the CSEM group at the University on
Michigan. The authors thank the reviewers for valuable comments.
NR 39
TC 16
Z9 16
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY 14
PY 2010
VL 115
AR A05207
DI 10.1029/2009JA014751
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 596TN
UT WOS:000277708500002
ER
PT J
AU Feng, M
McPhaden, MJ
Lee, T
AF Feng, Ming
McPhaden, Michael J.
Lee, Tong
TI Decadal variability of the Pacific subtropical cells and their influence
on the southeast Indian Ocean
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MERIDIONAL OVERTURNING CIRCULATION; INDONESIAN THROUGHFLOW; LEEUWIN
CURRENT
AB Historical sea level records reveal that a strengthening of the Pacific subtropical cells (STCs) since the early-1990's has reversed a multi-decadal weakening tendency. Stronger STCs correspond to a stronger Leeuwin Current in the southeast Indian Ocean (SEIO) and a stronger Indonesian Throughflow, due to dynamic connections of the Pacific and SEIO through equatorial and coastal waveguides. Multi-decadal trends of the STCs and their influence on the SEIO have confounded the detection of human induced global change signals in the short instrumental records of the two circulation systems. Citation: Feng, M., M. J. McPhaden, and T. Lee (2010), Decadal variability of the Pacific subtropical cells and their influence on the southeast Indian Ocean, Geophys. Res. Lett., 37, L09606, doi:10.1029/2010GL042796.
C1 [Feng, Ming] CSIRO Marine & Atmospher Res, Floreat, WA 6014, Australia.
[Lee, Tong] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
[McPhaden, Michael J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
RP Feng, M (reprint author), CSIRO Marine & Atmospher Res, Underwood Ave, Floreat, WA 6014, Australia.
EM ming.feng@csiro.au
RI Feng, Ming/F-5411-2010; McPhaden, Michael/D-9799-2016
OI Feng, Ming/0000-0002-2855-7092;
FU CSIRO; WAMSI; NOAA; NASA
FX We thank Gary Meyers and Lidia Pigot for providing the IX1 XBT data.
Tidal gauge sea level data are obtained from National Tidal Facility of
Australia and University of Hawaii Sea Level Center. This research is
sponsored by CSIRO and WAMSI, and partially supported by NOAA's Climate
Program Office and NASA Physical Oceanography Program. We would thank
two anonymous reviewers for constructive comments.
NR 21
TC 55
Z9 56
U1 1
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 MAY 13
PY 2010
VL 37
AR L09606
DI 10.1029/2010GL042796
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 596SC
UT WOS:000277704600003
ER
PT J
AU Dong, SF
Gille, ST
Sprintall, J
Fetzer, EJ
AF Dong, Shenfu
Gille, Sarah T.
Sprintall, Janet
Fetzer, Eric J.
TI Assessing the potential of the Atmospheric Infrared Sounder (AIRS)
surface temperature and specific humidity in turbulent heat flux
estimates in the Southern Ocean
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID BULK PARAMETERIZATION; SEA FLUXES; WIND-SPEED; AIRS/AMSU/HSB; RETRIEVAL;
CLOUDS
AB Surface air temperature (T-A), sea surface temperature (T-O), and surface specific humidity (q(a)) satellite retrievals from the Atmospheric Infrared Sounder (AIRS) are compared with shipboard measurements across Drake Passage for the period from September 2002 to June 2007. The objective is to evaluate whether AIRS retrievals, in conjunction with microwave sea surface temperatures from the Advanced Microwave Scanning Radiometer (AMSRE), can provide sufficiently accurate parameters to estimate sensible and latent heat fluxes in the data-limited Southern Ocean. The collocated data show that both AIRS T-A and T-O are colder than those from shipboard measurements, with a time mean bias of -2.03 degrees C for TA and -0.22 degrees C for T-O. Results show that air-sea temperature difference (T-A-T-O), q(a), and relative humidity (RH) are the major factors contributing to the differences between satellite and shipboard temperature measurements. Differences in AIRS and shipboard T-A (Delta T-A) decrease with increasing T-A-T-O, and Delta T-A increases with increasing RH, whereas differences in AIRS and shipboard T-O (Delta T-O) increase with both increasing T-A-T-O and increasing q(a). The time mean q(a) from AIRS is lower than the shipboard qa by 0.69 g/ kg. Statistical analyses suggest that T-A-T-O, cloud, and q(a) are the major contributors to the qa difference (Delta q(a)). Delta q(a) becomes more negative with increasing T-A-T-O and increasing cloud fraction. Delta q(a) also becomes more negative as q(a) increases. Compared with T-A, T-O, and T-A -T-O, from the National Centers for Environmental Prediction/National Center for Atmospheric Research Reanalysis (NCEP), AIRS-derived and AMSRE-derived variables show more small-scale spatial structure, as is also typical of the ship observations. Although AIRS qa gives a better representation of the full range of values of shipboard qa, its deviation from shipboard qa is relatively large compared to NCEP q(a). Compared with several existing gridded flux products, turbulent fluxes estimated from AIRS and AMSRE data using bulk algorithms are better able to represent the full range of flux values estimated from shipboard parameters.
C1 [Dong, Shenfu] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Studies, Miami, FL 33149 USA.
[Gille, Sarah T.; Sprintall, Janet] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92037 USA.
[Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dong, SF (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Studies, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM shenfu.dong@noaa.gov
RI Gille, Sarah/B-3171-2012; Dong, Shenfu/I-4435-2013;
OI Dong, Shenfu/0000-0001-8247-8072; Gille, Sarah/0000-0001-9144-4368
NR 36
TC 12
Z9 12
U1 3
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD MAY 13
PY 2010
VL 115
AR C05013
DI 10.1029/2009JC005542
PG 16
WC Oceanography
SC Oceanography
GA 596SZ
UT WOS:000277707100003
ER
PT J
AU Lucas, LE
Waliser, DE
Murtugudde, R
AF Lucas, Lisanne E.
Waliser, Duane E.
Murtugudde, Raghu
TI Mechanisms governing sea surface temperature anomalies in the eastern
tropical Pacific Ocean associated with the boreal winter Madden-Julian
Oscillation
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID MIXED-LAYER MODEL; INTRASEASONAL VARIABILITY; EQUATORIAL PACIFIC;
NORTHERN SUMMER; KELVIN WAVES; EL-NINO; SIMULATION; RADIATION; WIND;
PRECIPITATION
AB The study objective is to explore the relationship between the Madden-Julian Oscillation (MJO) and intraseasonal sea surface temperature (SST) variability in the eastern tropical Pacific Ocean. Previous studies have illustrated the connection between MJO and the production of zonally large (> 2000 km), persistent (similar to weeks) SST anomalies. Those studies suggested that vertical processes, such as advection and entrainment, forced remotely by winds in the western Pacific (via Kelvin waves) may be the mechanism controlling SST changes. To overcome limitations in situ observations (e. g., sparse and missing data/quantities) and to develop a more comprehensive physical understanding, this study examines the relationship using an ocean general circulation model. A simulation was conducted in which the model was forced by idealized MJO conditions constructed from observed forcing fields. Analysis of the model simulation shows an equatorial Kelvin wave initiated in the western Pacific Ocean. However, analysis of the model's mixed layer temperature heat budget shows that in the eastern Pacific meridional advection plays the major role in the sea surface temperature change, 61.8% of the warming phase and 70.7% of the cooling phase percent heat budget. Zonal advection is the second most important term to the warming phase (20.5%) with the vertical advection and mixing term being second for the cooling phase (37.6%). In addition, the results indicate that the primary component of the meridional advection is the advection of the mean meridional temperature gradient by MJO-forced meridional current anomalies. The implications and caveats of these results are discussed in relationship to results in prior studies.
C1 [Lucas, Lisanne E.] SUNY Stony Brook, Inst Terr & Planetary Atmospheres, Stony Brook, NY 11794 USA.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Water & Carbon Cycles Grp, Pasadena, CA 91109 USA.
[Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
RP Lucas, LE (reprint author), NOAA, Climate Program Off, 1315 East West Hwy,Room 12712, Silver Spring, MD 20910 USA.
EM sandy.lucas@noaa.gov
FU [NAG5-11033]
FX This work was prepared in conjunction with the first author's
dissertation research at State University of New York at Stony Brook. In
this regard, the authors would like to thank Dong-Ping Wang, Robert
Wilson, and Minghua Zhang for their comments and suggestions on this
work. Support for this study was provided under grants NAG5-11033 (D. E.
W., L. E. L.) and Salinity, QUICKSCAT, TRMM, and Indian Ocean
Biogeochemistry grants (R. M.) as well as the National Science
Foundation under grant ATM-0094416 (D. E. W.). This study's analysis and
presentation benefited from the use of the NCAR Graphics Package and
Seaspace Corporation's TeraScan software system.
NR 47
TC 8
Z9 8
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD MAY 13
PY 2010
VL 115
AR C05012
DI 10.1029/2009JC005450
PG 21
WC Oceanography
SC Oceanography
GA 596SZ
UT WOS:000277707100001
ER
PT J
AU Adimi, F
Soebiyanto, RP
Safi, N
Kiang, R
AF Adimi, Farida
Soebiyanto, Radina P.
Safi, Najibullah
Kiang, Richard
TI Towards malaria risk prediction in Afghanistan using remote sensing
SO MALARIA JOURNAL
LA English
DT Article
ID SYSTEMS
AB Background: Malaria is a significant public health concern in Afghanistan. Currently, approximately 60% of the population, or nearly 14 million people, live in a malaria-endemic area. Afghanistan's diverse landscape and terrain contributes to the heterogeneous malaria prevalence across the country. Understanding the role of environmental variables on malaria transmission can further the effort for malaria control programme.
Methods: Provincial malaria epidemiological data (2004-2007) collected by the health posts in 23 provinces were used in conjunction with space-borne observations from NASA satellites. Specifically, the environmental variables, including precipitation, temperature and vegetation index measured by the Tropical Rainfall Measuring Mission and the Moderate Resolution Imaging Spectoradiometer, were used. Regression techniques were employed to model malaria cases as a function of environmental predictors. The resulting model was used for predicting malaria risks in Afghanistan. The entire time series except the last 6 months is used for training, and the last 6-month data is used for prediction and validation.
Results: Vegetation index, in general, is the strongest predictor, reflecting the fact that irrigation is the main factor that promotes malaria transmission in Afghanistan. Surface temperature is the second strongest predictor. Precipitation is not shown as a significant predictor, as it may not directly lead to higher larval population. Autoregressiveness of the malaria epidemiological data is apparent from the analysis. The malaria time series are modelled well, with provincial average R(2) of 0.845. Although the R2 for prediction has larger variation, the total 6-month cases prediction is only 8.9% higher than the actual cases.
Conclusions: The provincial monthly malaria cases can be modelled and predicted using satellite-measured environmental parameters with reasonable accuracy. The Third Strategic Approach of the WHO EMRO Malaria Control and Elimination Plan is aimed to develop a cost-effective surveillance system that includes forecasting, early warning and detection. The predictive and early warning capabilities shown in this paper support this strategy.
C1 [Adimi, Farida; Soebiyanto, Radina P.; Kiang, Richard] NASA, Goddard Space Flight Ctr, Global Change Data Ctr, Greenbelt, MD 20771 USA.
[Adimi, Farida] Wyle Informat Syst, Mclean, VA 22102 USA.
[Soebiyanto, Radina P.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Catonsville, MD 21228 USA.
[Safi, Najibullah] Afghan Minist Publ Hlth, Natl Malaria Leishmaniasis Control Programme, Kabul, Afghanistan.
RP Kiang, R (reprint author), NASA, Goddard Space Flight Ctr, Global Change Data Ctr, Greenbelt, MD 20771 USA.
EM richard.kiang@nasa.gov
FU NASA Applied Sciences Public Health Application Program
FX This study was supported by NASA Applied Sciences Public Health
Application Program. The authors are thankful for the data processing
assistance of Patricia Hrubiak. The views expressed herein are the
private ones of the authors and do not purport to represent those of the
NASA or the Government of Afghanistan.
NR 17
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U1 0
U2 6
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1475-2875
J9 MALARIA J
JI Malar. J.
PD MAY 13
PY 2010
VL 9
AR 125
DI 10.1186/1475-2875-9-125
PG 11
WC Infectious Diseases; Parasitology; Tropical Medicine
SC Infectious Diseases; Parasitology; Tropical Medicine
GA 604TP
UT WOS:000278301700001
PM 20465824
ER
PT J
AU Kress, BT
Mertens, CJ
Wiltberger, M
AF Kress, B. T.
Mertens, C. J.
Wiltberger, M.
TI Solar energetic particle cutoff variations during the 29-31 October 2003
geomagnetic storm
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID MAGNETIC-FIELD; RADIATION ENVIRONMENT; COSMIC-RADIATION; MODEL;
SIMULATIONS; RIGIDITIES; LFM
AB At low latitudes to midlatitudes the Earth's magnetic field usually shields the upper atmosphere and spacecraft in low Earth orbit from solar energetic particles (SEPs). During severe geomagnetic storms, distortion of the Earth's field suppresses geomagnetic shielding, allowing SEPs access to the midlatitudes. A case study of the 26-31 October 2003 solar-geomagnetic event is used to examine how a severe geomagnetic storm affects SEP access to the Earth. Geomagnetic cutoffs are numerically determined in model geomagnetic fields using code developed by the Center for Integrated Space Weather Modeling (CISM) at Dartmouth College. The CISM-Dartmouth geomagnetic cutoff model is being used in conjunction with the High Energy and Charge Transport code (HZETRN) at the NASA Langley Research Center to develop a real-time data-driven prediction of radiation exposure at commercial airline altitudes. In this work, cutoff rigidities are computed on global grids and along several high-latitude flight routes before and during the geomagnetic storm. It is found that significant variations in SEP access to the midlatitudes and high latitudes can occur on time scales of an hour or less in response to changes in the solar wind dynamic pressure and interplanetary magnetic field. The maximum suppression of the cutoff is similar to 1 GV occurring in the midlatitudes during the main phase of the storm. The cutoff is also significantly suppressed by the arrival of an interplanetary shock. The maximum suppression of the cutoff due to the shock is approximately one half of the maximum suppression during the main phase of the storm.
C1 [Kress, B. T.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab HB6127, Hanover, NH 03755 USA.
[Mertens, C. J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Kress, BT (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab HB6127, Hanover, NH 03755 USA.
EM bkress@dartmouth.edu
RI Wiltberger, Michael/B-8781-2008
OI Wiltberger, Michael/0000-0002-4844-3148
FU National Aeronautics and Space Administration [NNX07AO77G]; National
Science Foundation [ATM-0120950]
FX This material is based upon work supported by the National Aeronautics
and Space Administration issued through the Applied Sciences Program and
under grant NNX07AO77G issued through the LWS TR&T program. This
material is also based upon work supported by the STC Program of the
National Science Foundation under agreement ATM-0120950 Thank you to
Chia-Lin Huang at Boston University and Larry Kepko at the University of
New Hampshire for their help preparing the solar wind input file for the
TS05 and LFM MHD geomagnetic field models. The authors are very grateful
to their reviewers for assistance with this manuscript.
NR 36
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Z9 21
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD MAY 13
PY 2010
VL 8
AR S05001
DI 10.1029/2009SW000488
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 596TS
UT WOS:000277709000001
ER
PT J
AU Marmorino, GO
Holt, B
Molemaker, MJ
DiGiacomo, PM
Sletten, MA
AF Marmorino, George O.
Holt, Benjamin
Molemaker, M. Jeroen
DiGiacomo, Paul M.
Sletten, Mark A.
TI Airborne synthetic aperture radar observations of "spiral eddy" slick
patterns in the Southern California Bight
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID OCEAN SURFACE; EDDIES; FRONTS; IMAGES; SEA; BAY
AB Repeat sampling on hourly time scales using an airborne synthetic aperture radar (SAR) is used to investigate the occurrence and evolving characteristics of spiral-shaped slick patterns, commonly presumed to be indicators of submesoscale ocean eddies, in the area around Santa Catalina Island, California (similar to 33.4 degrees N, 118.4 degrees W). Simultaneous SAR imagery and boat survey data are examined over two similar to 5 h long periods spaced 3 days apart in April 2003. The SAR imagery reveals several spiral-like patterns, roughly 5 km in diameter, occurring downstream of the western end of Catalina. We believe that the most likely formation mechanism for these patterns is current-wake instability related to the flow of the Southern California Countercurrent along the north shore of Catalina. In one case, there is an observed cold-core eddy and vortex sheet attached to the tip of the island, similar to island-wake simulations done by Dong and McWilliams (2007). In another case, the SAR imagery shows a series of slick patterns that, at least initially, resemble spiral eddies, but the data show no clear evidence of actual ocean eddies being present either at depth or through a rotating surface expression. A speculation is that such features signify island-wake eddies that are relatively weak and dissipate quickly. An unexpected finding was how quickly a spiral slick pattern could deteriorate, suggesting a time scale for the surface feature of the order of only several hours. An implication of this result is that care is needed when interpreting a single satellite SAR imagery for evidence of active submesoscale eddies. Recommendations are made for future field studies.
C1 [Marmorino, George O.; Sletten, Mark A.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[DiGiacomo, Paul M.] NOAA NESDIS Ctr Satellite Applicat & Res, Camp Springs, MD 20746 USA.
[Holt, Benjamin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Molemaker, M. Jeroen] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Marmorino, GO (reprint author), USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
EM marmorino@nrl.navy.mil
RI DiGiac