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1. IMPACT DELIVERY OF VOLATILES AND ORGANIC MOLECULES TO EARTH

Author: C. F. CHYBA, T. C. OWEN, and W.-H. IP
Published: 2021

2. MWR: Microwave Radiometer for the Juno Mission to Jupiter

Author: J. G. Kempenaar, R. Williamson, M. S. Zawadski, J. K. Arballo, Neil Chamberlain, Behrouz Khayatian, T. C. Owen, B. R. Franklin, Paul G. Steffes, R. C. Hughes, M. A. Janssen, Sushil K. Atreya, Amadeo Bellotti, Jonathan I. Lunine, Richard Hodges, C. C. Wang, Scott Bolton, Sidharth Misra, Steven Levin, Andrew P. Ingersoll, Samuel Gulkis, Liming Li, K. A. Lee, Glenn S. Orton, E. Sarkissian, A. Ulloa-Severino, V. Vorperion, A. S. Sahakian, J. C. Chen, L. A. Jewell, P. J. Pingree, Henry A. Conley, Daniel Santos-Costa, D. Gautier, Michael Allison, Shannon Brown, Fabiano Oyafuso, M. S. Loo, Cheng Li, Douglas Dawson, F. Maiwald, J. E. Oswald, Damon Russell, William Hatch, E. T. Sunada, Virgil Adumitroaie, Richard Redick, A. S. Mazer, G. Bedrosian, and Amarit Kitiyakara
Subjects: Physics, 010504 meteorology & atmospheric sciences, Microwave radiometer, Atmosphere of Jupiter, Astronomy and Astrophysics, 01 natural sciences, Jovian, Jupiter, Atmosphere, Exploration of Jupiter, Space and Planetary Science, Brightness temperature, Physics::Space Physics, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Orbit insertion, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract: The Juno Microwave Radiometer (MWR) is a six-frequency scientific instrument designed and built to investigate the deep atmosphere of Jupiter. It is one of a suite of instruments on NASA’s New Frontiers Mission Juno launched to Jupiter on August 5, 2011. The focus of this paper is the description of the scientific objectives of the MWR investigation along with the experimental design, observational approach, and calibration that will achieve these objectives, based on the Juno mission plan up to Jupiter orbit insertion on July 4, 2016. With frequencies distributed approximately by octave from 600 MHz to 22 GHz, the MWR will sample the atmospheric thermal radiation from depths extending from the ammonia cloud region at around 1 bar to pressure levels as deep as 1000 bars. The primary scientific objectives of the MWR investigation are to determine the presently unknown dynamical properties of Jupiter’s subcloud atmosphere and to determine the global abundance of oxygen and nitrogen, present in the atmosphere as water and ammonia deep below their respective cloud decks. The MWR experiment is designed to measure both the thermal radiation from Jupiter and its emission-angle dependence at each frequency relative to the atmospheric local normal with high accuracy. The antennas at the four highest frequencies (21.9, 10.0, 5.2, and 2.6 GHz) have ∼12° beamwidths and will achieve a spatial resolution approaching 600 km near perijove. The antennas at the lowest frequencies (0.6 and 1.25 GHz) are constrained by physical size limitations and have 20° beamwidths, enabling a spatial resolution of as high as 1000 km to be obtained. The MWR will obtain Jupiter’s brightness temperature and its emission-angle dependence at each point along the subspacecraft track, over angles up to 60° from the normal over most latitudes, during at least six perijove passes after orbit insertion. The emission-angle dependence will be obtained for all frequencies to an accuracy of better than one part in 10^3, sufficient to detect small variations in atmospheric temperature and absorber concentration profiles that distinguish dynamical and compositional properties of the deep Jovian atmosphere.
Published: 2017

3. In situ measurement of atmospheric krypton and xenon on Mars with Mars Science Laboratory

Author: Susanne P. Schwenzer, Caroline Freissinet, Melissa G. Trainer, A. A. Pavlov, John H. Jones, Pamela G. Conrad, Michael H. Wong, Sushil K. Atreya, Roger C. Wiens, Robert O. Pepin, H. L. K. Manning, Paul R. Mahaffy, Charles Malespin, T. C. Owen, and Heather B. Franz
Subjects: Martian, 010504 meteorology & atmospheric sciences, Krypton, chemistry.chemical_element, Noble gas, Atmosphere of Mars, Mars Exploration Program, 01 natural sciences, Astrobiology, Geophysics, Xenon, chemistry, Meteorite, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Isotopes of xenon, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract: Mars Science Laboratory's Sample Analysis at Mars (SAM) investigation has measured all of the stable isotopes of the heavy noble gases krypton and xenon in the martian atmosphere, in situ, from the Curiosity Rover at Gale Crater, Mars. Previous knowledge of martian atmospheric krypton and xenon isotope ratios has been based upon a combination of the Viking mission's krypton and xenon detections and measurements of noble gas isotope ratios in martian meteorites. However, the meteorite measurements reveal an impure mixture of atmospheric, mantle, and spallation contributions. The xenon and krypton isotopic measurements reported here include the complete set of stable isotopes, unmeasured by Viking. The new results generally agree with Mars meteorite measurements but also provide a unique opportunity to identify various non-atmospheric heavy noble gas components in the meteorites. Kr isotopic measurements define a solar-like atmospheric composition, but deviating from the solar wind pattern at 80Kr and 82Kr in a manner consistent with contributions originating from neutron capture in Br. The Xe measurements suggest an intriguing possibility that isotopes lighter than 132Xe have been enriched to varying degrees by spallation and neutron capture products degassed to the atmosphere from the regolith, and a model is constructed to explore this possibility. Such a spallation component, however, is not apparent in atmospheric Xe trapped in the glassy phases of martian meteorites.
Published: 2016

4. MWR: Microwave Radiometer for the Juno Mission to Jupiter

Author: M. A. Janssen, J. E. Oswald, S. T. Brown, S. Gulkis, S. M. Levin, S. J. Bolton, M. D. Allison, S. K. Atreya, D. Gautier, A. P. Ingersoll, J. I. Lunine, G. S. Orton, T. C. Owen, P. G. Steffes, V. Adumitroaie, A. Bellotti, L. A. Jewell, C. Li, L. Li, S. Misra, F. A. Oyafuso, D. Santos-Costa, E. Sarkissian, R. Williamson, J. K. Arballo, A. Kitiyakara, A. Ulloa-Severino, J. C. Chen, F. W. Maiwald, A. S. Sahakian, P. J. Pingree, K. A. Lee, A. S. Mazer, R. Redick, R. E. Hodges, R. C. Hughes, G. Bedrosian, D. E. Dawson, W. A. Hatch, D. S. Russell, N. F. Chamberlain, M. S. Zawadski, B. Khayatian, B. R. Franklin, H. A. Conley, J. G. Kempenaar, M. S. Loo, E. T. Sunada, V. Vorperion, and C. C. Wang
Published: 2017

5. The Juno Mission

Author: S. J. Bolton, J. Lunine, D. Stevenson, J. E. P. Connerney, S. Levin, T. C. Owen, F. Bagenal, D. Gautier, A. P. Ingersoll, G. S. Orton, T. Guillot, W. Hubbard, J. Bloxham, A. Coradini, S. K. Stephens, P. Mokashi, R. Thorne, and R. Thorpe
Published: 2017

6. Xenon isotopes in 67P/Churyumov-Gerasimenko show that comets contributed to Earth's atmosphere

Author: E. Kopp, Stephen A. Fuselier, Michael R. Combi, Chia-Yu Tzou, Thierry Sémon, André Bieler, Myrtha Hässig, Bernard Marty, David V. Bekaert, Martin Rubin, Sébastien Gasc, C. Briois, Peter Wurz, Annette Jäckel, Ulrich Mall, Akiva Bar-Nun, Kirk C. Hansen, J. De Keyser, Ursina Calmonte, Kathrin Altwegg, A. Korth, Hans Balsiger, T. C. Owen, Léna Le Roy, J. H. Waite, Jean-Jacques Berthelier, Olivier Mousis, Henri Rème, B. Fiethe, Tamas I. Gombosi, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Center for Space and Habitability (CSH), University of Bern, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Department of Geophysics [Tel Aviv] (TAU), Tel Aviv University (TAU), Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Science and Engineering Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA) PRODEX program (Programme de Développement d’Expériences Scientifiques), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 267255,EC:FP7:ERC,ERC-2010-AdG_20100224,NOGAT(2011), Universität Bern [Bern], Department of Geosciences [Tel Aviv], Tel Aviv University [Tel Aviv], Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Max-Planck-Institut für Sonnensystemforschung (MPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherches Pétrographiques et Géochimiques ( CRPG ), Université de Lorraine ( UL ) -Centre National de la Recherche Scientifique ( CNRS ), Center for Space and Habitability ( CSH ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Climate and Space Sciences and Engineering ( CLaSP ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] ( SwRI ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES ), University of Hawaii at Manoa ( UHM ), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: 010504 meteorology & atmospheric sciences, 530 Physics, Physics::Instrumentation and Detectors, Comet, chemistry.chemical_element, 01 natural sciences, law.invention, Astrobiology, Atmosphere, Orbiter, Xenon, law, 540 Chemistry, 0103 physical sciences, Isotopes of xenon, Physics::Atomic and Molecular Clusters, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Multidisciplinary, Isotope, Spectrometer, 520 Astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 620 Engineering, Atmosphere of Earth, chemistry, 13. Climate action, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, [ SDU ] Sciences of the Universe [physics]
Abstract: Comets contributed to Earth's atmosphere Models of xenon's origin in Earth's atmosphere require an additional, unknown source that has been a mystery for several decades. Marty et al. measured isotopic ratios of xenon released from comet 67P/Churyumov-Gerasimenko and found that they match the heretofore unknown source. The xenon appears to have been trapped in ice within the comet since before the solar system formed. Comets contributed about a quarter of the xenon on Earth, which constrains the amount of other materials (such as water) delivered to our planet by comets. Science , this issue p. 1069
Published: 2017

7. Hydrocarbons on Saturn's satellites Iapetus and Phoebe

Author: Dale P. Cruikshank, Yvonne J. Pendleton, C. M. Dalle Ore, Bonnie J. Buratti, Robert H. Brown, Gianrico Filacchione, Fabrizio Capaccioni, Eric Wegryn, Giancarlo Bellucci, Vito Mennella, Priscilla Cerroni, Vittorio Formisano, P. D. Nicholson, Roger N. Clark, Pierre Drossart, M. Combes, T. C. Owen, Yves Langevin, Robert M. Nelson, T. B. McCord, Ralf Jaumann, Kevin H. Baines, Dennis L. Matson, Bruno Sicardy, Angioletta Coradini, Jean-Pierre Bibring, Christophe Sotin, SETI Institute, NASA Ames Research Center, Moffett Field, Search for Extraterrestrial Intelligence Institute (SETI), Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Jet Propulsion Laboratory, California Institute of Technology (JPL), US Geological Survey, Denver, Space Science Institute, Winthrop, Department of Astronomy, Cornell University, Institute for Astronomy, University of Hawaii, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Roma), Department of Planetary Exploration, DLR, Université de Nantes (UN), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC)
Subjects: spectroscopy, Solar System, Materials science, Iapetus, Astronomy and Astrophysics, organic chemistry, Astrobiology, Interstellar medium, Meteorite, Space and Planetary Science, Geometric albedo, Absorption band, Saturn, Circumstellar dust, satellites composition, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmic dust
Abstract: Material of low geometric albedo (pV⩽0.1pV⩽0.1) is found on many objects in the outer Solar System, but its distribution in the saturnian satellite system is of special interest because of its juxtaposition with high-albedo ice. In the absence of clear, diagnostic spectral features, the composition of this low-albedo (or “dark”) material is generally inferred to be carbon-rich, but the form(s) of the carbon is unknown. Near-infrared spectra of the low-albedo hemisphere of Saturn's satellite Iapetus were obtained with the Visible–Infrared Mapping Spectrometer (VIMS) on the Cassini spacecraft at the fly-by of that satellite of 31 December 2004, yielding a maximum spatial resolution on the satellite's surface of ∼65 km. The spectral region 3–3.6 μm reveals a broad absorption band, centered at 3.29 μm, and concentrated in a region comprising about 15% of the low-albedo surface area. This is identified as the CH stretching mode vibration in polycyclic aromatic hydrocarbon (PAH) molecules. Two weaker bands attributed to CH2 stretching modes in aliphatic hydrocarbons are found in association with the aromatic band. The bands most likely arise from aromatic and aliphatic units in complex macromolecular carbonaceous material with a kerogen- or coal-like structure, similar to that in carbonaceous meteorites. VIMS spectra of Phoebe, encountered by Cassini on 11 June 2004, also show the aromatic hydrocarbon band, although somewhat weaker than on Iapetus. The origin of the PAH molecular material on these two satellites is unknown, but PAHs are found in carbonaceous meteorites, cometary dust particles, circumstellar dust, and interstellar dust.
Published: 2008

8. Surface composition and temperature of the TNO Orcus

Author: A. Guilbert, C. de Bergh, Olivier Hainaut, Angioletta Coradini, Alain Doressoundiram, T. C. Owen, Christophe Dumas, Alvaro Alvarez-Candal, F. Merlin, M. A. Barucci, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), European Southern Observatory, Institute for Astronomy, University of Hawaii, Istituto di Fisica dello Spazio Interplanetario (IFSI), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)
Subjects: Physics, Very Large Telescope, education.field_of_study, Population, Astronomy and Astrophysics, Astrophysics, Methods observational, Astrobiology, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Water ice, Trans-Neptunian object, Formation and evolution of the Solar System, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], education, Chemical composition
Abstract: International audience; Aims:The aim of this paper is to investigate the surface composition of the Transneptunian Object (TNO) Orcus. Methods: High quality observations have been carried out with the new instrument SINFONI at the Very Large Telescope (VLT) of ESO. Results: Crystalline water ice, and possibly ammonia ice, have been found from spectroscopic observations of the TNO Orcus between 1.4 and 2.4 mum. Conclusions: The existence of such ices on the surface of Orcus may indicate a renewal mechanism on the surface and geological activity. The presence of ammonia on the surface of Orcus, if confirmed, could have important implications for the composition of the primitive solar nebula and the formation of the TNO population.
Published: 2008

9. Trapping of N2, CO and Ar in amorphous ice—Application to comets

Author: Akiva Bar-Nun, T. C. Owen, and G. Notesco
Subjects: Physics, Solar System, Space and Planetary Science, Comet, Amorphous ice, Astronomy and Astrophysics, Water ice, High resolution spectra, Trapping, Astrophysics, Amorphous solid
Abstract: Recent attempts using high resolution spectra to detect N+2 in several comets were unsuccessful [Cochran, A.L., Cochran, W.D., Baker, E.S., 2000. Icarus 146, 583–593; Cochran, A.L., 2002. Astrophys. J. 576, L165–L168]. The upper limits on N+2 in comparison with the positively detected CO+ for Comets C/1995 O1 Hale–Bopp, 122P/1995 S1 de Vico and 153P/2002 C1 Ikeya–Zhang range between N 2 + /CO + ( 0.65 – 5.4 ) × 10 −4 . Ar was not detected in three recent comets [Weaver, H.A., Feldman, P.D., Combi, M.R., Krasnopolsky, V., Lisse, C.M., Shemansky, D.E., 2002. Astrophys. J. 576, L95–L98], with upper limits of Ar/CO ( 3.4 – 7.8 ) × 10 −2 for Comets C/1999 T1 McNaught–Hartley, C/2001 A2 LINEAR and C/2000 WM1 LINEAR. The Ar detected by Stern et al. [Stern, S.A., Slater, D.C., Festou, M.C., Parker, J.Wm., Gladstone, G.R., A'Hearn, M.F., Wilkinson, E., 2000. Astrophys. J. 544, L169–L172] for Comet C/1995 O1 Hale–Bopp, gives a ratio Ar/CO = 7.25 × 10 −2 , which was not confirmed by Cosmovici et al. [Cosmovici, C.B., Bratina, V., Schwarz, G., Tozzi, G., Mumma, M.J., Stalio, R., 2006. Astrophys. Space Sci. 301, 135–143]. Trying to solve the two problems, we studied experimentally the trapping of N 2 + CO + Ar in amorphous water ice, at 24–30 K. CO was found to be trapped in the ice 20–70 times more efficiently than N2 and with the same efficiency as Ar. The resulting Ar/CO ratio of 1.2 × 10 −2 is consistent with Weaver et al.'s [Weaver, H.A., Feldman, P.D., Combi, M.R., Krasnopolsky, V., Lisse, C.M., Shemansky, D.E., 2002. Astrophys. J. 576, L95–L98] non-detection of Ar. However, with an extreme starting value for N2/CO = 0.22 in the region where the ice grains which agglomerated to produce comet nuclei were formed, the expected N2/CO ratio in the cometary ice should be 6.6 × 10 −3 , much higher than its non-detection limit.
Published: 2007

10. The imprint of atmospheric evolution in the D/H of Hesperian clay minerals on Mars

Author: Pamela G. Conrad, Daniel P. Glavin, Rafael Navarro-González, Paul R. Mahaffy, A. A. Pavlov, Amy McAdam, Shawn Domagal-Goldman, Jennifer C. Stern, Melissa G. Trainer, A. E. Brunner, J. L. Eigenbrode, Sushil K. Atreya, Christopher R. Webster, H. B. Franz, D. W. Ming, Kenneth H. Williford, John P. Grotzinger, G. Flesch, Charles Malespin, Caroline Freissinet, James J. Wray, Lance E. Christensen, Andrew Steele, T. C. Owen, L. A. Leshin, Paul B. Niles, and John H. Jones
Subjects: Martian, Multidisciplinary, Hydrogen, MSL-Radiation, chemistry.chemical_element, Mars, Atmosphere of Mars, Mars Exploration Program, Gale crater, Astrobiology, chemistry, Impact crater, Sample Analysis at Mars, D/H ratio, Hesperian, Clay minerals, Geology
Abstract: Of water and methane on Mars The Curiosity rover has been collecting data for the past 2 years, since its delivery to Mars (see the Perspective by Zahnle). Many studies now suggest that many millions of years ago, Mars was warmer and wetter than it is today. But those conditions required an atmosphere that seems to have vanished. Using the Curiosity rover, Mahaffy et al. measured the ratio of deuterium to hydrogen in clays that were formed 3.0 to 3.7 billion years ago. Hydrogen escapes more readily than deuterium, so this ratio offers a snapshot measure of the ancient atmosphere that can help constrain when and how it disappeared. Most methane on Earth has a biological origin, so planetary scientists have keenly pursued its detection in the martian atmosphere as well. Now, Webster et al. have precisely confirmed the presence of methane in the martian atmosphere with the instruments aboard the Curiosity rover at Gale crater. Science , this issue p. 412 , p. 415 ; see also p. 370
Published: 2015

11. Molecular nitrogen in comet 67P/Churyumov-Gerasimenko indicates a low formation temperature

Author: T. C. Owen, Henri Rème, Martin Rubin, Sébastien Gasc, Frederik Dhooghe, Jean-Jacques Berthelier, Peter Wurz, Léna Le Roy, Ulrich Mall, Michael R. Combi, Ursina Calmonte, Thierry Sémon, E. Kopp, Annette Jäckel, C. Briois, Kirk C. Hansen, A. Korth, André Bieler, J. De Keyser, Stephen A. Fuselier, Olivier Mousis, J. H. Waite, Chia-Yu Tzou, B. Fiethe, Tamas I. Gombosi, Peter Eberhardt, Akiva Bar-Nun, Kathrin Altwegg, Myrtha Hässig, Bernard Marty, Hans Balsiger, Peter Bochsler, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Center for Space and Habitability (CSH), University of Bern, Department of Geophysics [Tel Aviv] (TAU), Tel Aviv University (TAU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), PRODEX/ROSINA PEA 90020., ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project: 267255,EC:FP7:ERC,ERC-2010-AdG_20100224,NOGAT(2011), Universität Bern [Bern], Center for Space and Habitability ( CSH ), Department of Geosciences [Tel Aviv], Tel Aviv University [Tel Aviv], IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] ( SwRI ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Centre de Recherches Pétrographiques et Géochimiques ( CRPG ), Université de Lorraine ( UL ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES ), University of Hawaii at Manoa ( UHM ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), ANR-11-IDEX-0001-02,A*MIDEX,Projet Investissements d'Avenir ( 2012 ), European Project : 267255,EC:FP7:ERC,ERC-2010-AdG_20100224,NOGAT ( 2011 ), Max-Planck-Institut für Sonnensystemforschung (MPS), Université de Lorraine (UL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Solar System, Nebula, Multidisciplinary, Spectrometer, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, [ SDU.STU.GC ] Sciences of the Universe [physics]/Earth Sciences/Geochemistry, Nitrogen, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrobiology, Jupiter, Pluto, chemistry, 13. Climate action, Planet, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry
Abstract: Making comets in the cold The speciation of nitrogen compounds in comets can tell us about their history. Comets are some of the most ancient bodies in the solar system and should contain the nitrogen compounds that were abundant when they formed. Using the ROSINA mass spectrometer aboard the Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko, Rubin et al. found molecular nitrogen at levels that are depleted compared to those in the primordial solar system. Depletion of such a magnitude suggests that the comet formed either from the low-temperature agglomeration of pristine amorphous water ice grains or from clathrates. Science , this issue p. 232
Published: 2015

12. 67P/Churyumov-Gerasimenko, a Jupiter family comet with a high D/H ratio

Author: Sébastien Gasc, Ulrich Mall, E. Kopp, Kathrin Altwegg, J. De Keyser, Michael R. Combi, Thierry Sémon, Peter Bochsler, Eddy Neefs, Jean-Jacques Berthelier, Bernard Marty, Hans Balsiger, Annette Jäckel, Henri Rème, T. C. Owen, Peter Eberhardt, A. Korth, Peter Wurz, Christelle Briois, Olivier Mousis, Stephen A. Fuselier, Lena Leroy, Chia-Yu Tzou, H. Waite, André Bieler, Martin Rubin, Myrtha Hässig, Kirk C. Hansen, Ursina Calmonte, Akiva Bar-Nun, B. Fiethe, Tamas I. Gombosi, Physikalisches Institut [Bern], Universität Bern [Bern], Department of Geosciences [Tel Aviv], Tel Aviv University [Tel Aviv], IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), University of Michigan [Ann Arbor], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Space Science Division [San Antonio], Southwest Research Institute [San Antonio] ( SwRI ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Centre de Recherches Pétrographiques et Géochimiques ( CRPG ), Université de Lorraine ( UL ) -Centre National de la Recherche Scientifique ( CNRS ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), University of Hawaii, Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), PRODEX/ROSINA PEA 90020, CNES, European Project : 267255,EC:FP7:ERC,ERC-2010-AdG_20100224,NOGAT ( 2011 ), Universität Bern [Bern] (UNIBE), Department of Geophysics [Tel Aviv] (TAU), Tel Aviv University (TAU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan System-University of Michigan System, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] (SwRI), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Project: 267255,EC:FP7:ERC,ERC-2010-AdG_20100224,NOGAT(2011), Max-Planck-Institut für Sonnensystemforschung (MPS), Université de Lorraine (UL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Multidisciplinary, Spacecraft, business.industry, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, [ SDU.STU.GC ] Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrobiology, Jupiter, 13. Climate action, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, Terrestrial planet, business, Earth (classical element)
Abstract: The provenance of water and organic compounds on Earth and other terrestrial planets has been discussed for a long time without reaching a consensus. One of the best means to distinguish between different scenarios is by determining the deuterium-to-hydrogen (D/H) ratios in the reservoirs for comets and Earth’s oceans. Here, we report the direct in situ measurement of the D/H ratio in the Jupiter family comet 67P/Churyumov-Gerasimenko by the ROSINA mass spectrometer aboard the European Space Agency’s Rosetta spacecraft, which is found to be (5.3 ± 0.7) × 10 −4 —that is, approximately three times the terrestrial value. Previous cometary measurements and our new finding suggest a wide range of D/H ratios in the water within Jupiter family objects and preclude the idea that this reservoir is solely composed of Earth ocean–like water.
Published: 2015

13. Failure of Conservative Management After the Passage of a Distal Colonic 'Cast': Report of a Case

Author: Claire J. Taylor, Eoghan R T C Owen, Hilary A. Birch, M. Aslam, Charlotte Foley, and Kalakata Reddy
Subjects: medicine.medical_specialty, Colon, medicine.medical_treatment, Rectum, Colonoscopy, Ischemic colitis, Diverticulitis, Colonic, Laparotomy, medicine, Humans, Treatment Failure, Intestinal Mucosa, Abscess, Aged, medicine.diagnostic_test, business.industry, Gastroenterology, General Medicine, Diverticulitis, medicine.disease, Colorectal surgery, Endoscopy, Surgery, medicine.anatomical_structure, Infarction, Female, business, Colitis, Ischemic, Intestinal Obstruction
Abstract: The spontaneous passage per rectum of a full-thickness colon “cast” is a rare consequence of acute colonic ischemia. Previous cases have undergone surgery soon afterward because of intractable symptoms. We report a patient who was managed conservatively for 11 months but ultimately required definitive surgery. The clinical, radiographic, pathologic, and endoscopic findings were obtained from the case notes and compared with previously reported cases. A 67-year-old obese patient underwent a Hartmann’s procedure for a perforated diverticular abscess, which was reversed six months later. On the first postoperative night after the reversal, she had a brief hypotensive episode, and three weeks later passed a 21-cm, full-thickness infarcted piece of colon. She did not develop peritonitis and for 11 months experienced only mild symptoms. Under colonoscopic surveillance, the granulation tissue conduit connecting the remaining viable bowel became increasingly stenosed proximally and difficult to dilate. After three rapidly consecutive episodes of large-bowel obstruction, she required a laparotomy to resect the stricture and restore bowel continuity. From a literature review, this is the eighth case of its kind and the first in which such prolonged conservative management has been possible. When symptoms permit, it is feasible to manage patients conservatively in the short-term after this unusual event to allow recovery from the initial insult and planning of future surgery. However, definitive treatment is surgical and colonoscopic management should not delay this once the patient is fit for surgery.
Published: 2005

14. Exploring The Saturn System In The Thermal Infrared: The Composite Infrared Spectrometer

Author: Gordon L. Bjoraker, John R. Spencer, Glenn S. Orton, Barney J. Conrath, Peter J. Gierasch, Mian M. Abbas, R. K. Achterberg, D. E. Jennings, J. P. Meyer, F. M. Flasar, T. C. Owen, Angioletta Coradini, M. D. Smith, Fredric W. Taylor, Renée Prangé, John C. Pearl, K. Grossman, Conor A. Nixon, S. Edberg, Peter A. R. Ade, A. A. Mamoutkine, Thierry Fouchet, A. Marten, Mark R. Showalter, M. E. Segura, Chiara Ferrari, D. Gautier, Amy A. Simon-Miller, C. J. Cesarsky, John C. Brasunas, Athena Coustenis, Patrick G. J. Irwin, R. W. Carlson, Régis Courtin, Scott G. Edgington, Linda Spilker, Robert E. Samuelson, E. Lellouch, François Raulin, Paul N. Romani, Peter L. Read, Antonella Barucci, V. G. Kunde, S. B. Calcutt, B. Bezard, Goddard Space Flight Center, NASA, Astrophysics Science Division, University of Maryland, Marshall Space Flight Center, NASA, Science Systems and Applications Inc, Cardiff University, Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Oxford University, European Southern Observatory (ESO), Department of Astronomy, Cornell University, Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Roma), Jet Propulsion Laboratory, California Institute of Technology (JPL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Gesamthochschule Wuppertal, University of Hawaii, Hilo, Université Paris Cité (UPCité), QSS Group, Stanford University, and Southwest Research Institute
Subjects: Physics, business.industry, Rings of Saturn, Michelson interferometer, Astronomy and Astrophysics, Field of view, law.invention, Interferometry, symbols.namesake, Optics, Far infrared, Space and Planetary Science, law, Physics::Space Physics, symbols, Astronomical interferometer, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Titan (rocket family), business
Abstract: International audience; The Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer (FTS) on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 cm- 1 (1 mm to 7mu m), with a spectral resolution that can be set from 0.5 to 15.5 cm- 1. The far infrared portion of the spectrum (10 600 cm- 1) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view (FOV). The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600 1100 cm- 1, 1100 1400 cm- 1). Each focal plane is composed of a 1× 10 array of HgCdTe detectors, each detector having a 0.3-mrad FOV. CIRS observations will provide three-dimensional maps of temperature, gas composition, and aerosols/condensates of the atmospheres of Titan and Saturn with good vertical and horizontal resolution, from deep in their tropospheres to high in their mesospheres. CIRS's ability to observe atmospheres in the limb-viewing mode (in addition to nadir) offers the opportunity to provide accurate and highly resolved vertical profiles of these atmospheric variables. The ability to observe with high-spectral resolution should facilitate the identification of new constituents. CIRS will also map the thermal and compositional properties of the surfaces of Saturn's icy satellites. It will similarly map Saturn's rings, characterizing their dynamical and spatial structure and constraining theories of their formation and evolution. The combination of broad spectral range, programmable spectral resolution, the small detector fields of view, and an orbiting spacecraft platform will allow CIRS to observe the Saturnian system in the thermal infrared at a level of detail not previously achieved.
Published: 2004

15. The Nitrogen Isotopic Ratio in Jupiter’s Atmosphere from Observations by the Composite Infrared Spectrometer on theCassiniSpacecraft

Author: A. LeClair, Gordon L. Bjoraker, F. M. Flasar, Mian M. Abbas, Conor A. Nixon, G. S. Orton, V. G. Kunde, R. K. Achterberg, Barney J. Conrath, Paul N. Romani, D. J. Jennings, and T. C. Owen
Subjects: Physics, Infrared, Atmosphere of Jupiter, Galileo Probe, Astronomy, Infrared spectroscopy, Astronomy and Astrophysics, Astrophysics, Spectral line, Jupiter, Atmosphere, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System, Astrophysics::Galaxy Astrophysics
Abstract: The Composite Infrared Spectrometer (CIRS) on the Cassini spacecraft made infrared observations of Jupiter's atmosphere during the flyby in December 2000 to January 2001. The unique database in the 600-1400/cm region with 0.53 and 2.8/cm spectral resolutions obtained from the observations permits retrieval of global maps of the thermal structure and composition of Jupiter's atmosphere including the distributions of (14)NH3 and (15)NH3. Analysis of Jupiter's ammonia distributions from three isolated (15)NH3 spectral lines in eight latitudes is presented for evaluation of the nitrogen isotopic ratio. The nitrogen isotopic ratio (14)N/(15)N (or (15)N/(14)N) in Jupiter's atmosphere in this analysis is calculated to be: 448 +/- 62 ((2.23 +/- 0.31) x 10(exp -3)). This value of the ratio determined from CIRS data is found to be in very close agreement with the value previously obtained from the measurements by the Galileo Probe Mass Spectrometer. Some possible mechanisms to account for the variation of Jupiter's observed isotopic ratio relative to various astrophysical environments are discussed.
Published: 2004

16. Short-wavelength infrared (1.3–2.6 μm) observations of the nucleus of Comet 19P/Borrelly

Author: Bonnie J. Buratti, Laurence A. Soderblom, Roger V. Yelle, Randolph L. Kirk, T. C. Owen, Robert H. Brown, and Daniel T. Britt
Subjects: Materials science, Infrared, Comet, Imaging spectrometer, Astronomy, Infrared spectroscopy, Astronomy and Astrophysics, Astrophysics, Spectral line, Wavelength, medicine.anatomical_structure, Space and Planetary Science, Absorption band, medicine, Nucleus
Abstract: During the last two minutes before closest approach of Deep Space 1 to Comet 19P/Borrelly, a long exposure was made with the short-wavelength infrared (SWIR) imaging spectrometer. The observation yielded 46 spectra covering 1.3–2.6 μm; the footprint of each spectrum was ∼160 m × width of the nucleus. Borrelly's highly variegated and extremely dark 8-km-long nucleus exhibits a strong red slope in its short-wavelength infrared reflection spectrum. This slope is equivalent to J–K and H–K colors of ∼0.82 and ∼0.43, respectively. Between 2.3–2.6 μm thermal emission is clearly detectable in most of the spectra. These data show the nucleus surface to be hot and dry; no trace of H2O ice was detected. The surface temperature ranged continuously across the nucleus from ⩽300 K near the terminator to a maximum of ∼340 K, the expected sub-solar equilibrium temperature for a slowly rotating body. A single absorption band at ∼2.39 μm is quite evident in all of the spectra and resembles features seen in nitrogen-bearing organic molecules that are reasonable candidates for compositional components of cometary nuclei. However as of yet the source of this band is unknown.
Published: 2004

17. Gas trapping in water ice at very low deposition rates and implications for comets

Author: G. Notesco, Akiva Bar-Nun, and T. C. Owen
Subjects: Argon, Ice formation, Materials science, Analytical chemistry, chemistry.chemical_element, Astronomy and Astrophysics, Mars Exploration Program, Trapping, Astrobiology, chemistry, Orders of magnitude (specific energy), Space and Planetary Science, Water ice, Deposition (chemistry), Earth (classical element)
Abstract: The effect of water ice formation temperature and rate of ice deposition on a cold plate on the amount of trapped argon (equivalent to CO), and the ratios of Ar/Kr/Xe trapped in the water ice were studied at 50, 27 and 22 K and at ice formation rates ranging over four orders of magnitude, from 10−1 to 10−5 μm min−1. Contrary to our previous conclusions that cometary ices were formed at 50–60 K, we now conclude that these ices were formed at about 25 K. At 25 K the enrichment ratios for Ar, Kr, and Xe remained the same as those at 50 K, reinforcing our suggestion of cometary contribution of these noble gases to the atmospheres of Earth and Mars.
Published: 2003

18. [Untitled]

Author: D. McGonagle, Thomas B. Lowe, Per Bergman, Henry E. Matthews, William M. Irvine, A. Nummelin, and T. C. Owen
Subjects: Meteoroid, Hydrogen isocyanide, Comet, Photodissociation, Hydrogen cyanide, Astronomy, General Medicine, Astrophysics, Organic molecules, Prebiotic chemistry, chemistry.chemical_compound, chemistry, Space and Planetary Science, Ecology, Evolution, Behavior and Systematics
Abstract: Comets have been suggested as a possibly significant source of organic molecules to the early Earth. Hydrogen cyanide (HCN) is important in models of prebiotic chemistry, but may be difficult to form in the early terrestrial environment, while hydrogen isocyanide (HNC) is a 'classical' tracer of interstellar ion-molecule chemistry. We have observed both HCN and HNC in 2 recent comets, bringing the number of comets with published measurements of the HNC/HCN abundance ratio to 6. The HNC/HCN ratio in comet Ikeya-Zhang appears to increase with decreasing heliocentric distance, as was previously observed for comet Hale-Bopp, indicating that the HNC is produced at least in part by processes in the cometary coma (atmosphere) and is not simply a constituent of the nuclear ices. Both comets C/2000 WMI (Linear) and C/2002 C1 (Ikeya-Zhang) exhibit values of the HNC/HCN ratio that appear to be too large (approximately 0.09-0.19) to be matched by current models of coma chemistry. Cometary HNC may be a photodissociation product of organic grains or large organic polymers stored in the nucleus. We have also set a limit on the emission from the NO radical in comet WM1.
Published: 2003

19. 10 Hygiea: ISO Infrared Observations

Author: Alain Doressoundiram, M. C. De Sanctis, Patrick W. Morris, Vito Mennella, T. G. Müller, E. Dotto, M. A. Barucci, John Robert Brucato, T. C. Owen, Jacques Crovisier, Luigi Colangeli, M. Fulchignoni, A. Le Bras, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Physics, Spectrometer, Infrared, Astronomy, Astronomy and Astrophysics, Astrophysics, Spectral line, Wavelength, Space and Planetary Science, Asteroid, Chondrite, Emissivity, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectroscopy, Astrophysics::Galaxy Astrophysics
Abstract: Observations of emissivity features of 10 Hygiea have been made for the first time in the relatively unexplored thermal-infrared wavelength region with the ISO (Infrared Space Observatory) satellite. Spectrophotomer (PHT-S) and short wavelength spectrometer (SWS) spectra of 10 Hygiea, obtained at 5.8–11.6 and 7–45 μm, respectively, are presented. In order to remove the thermal emission continuum, an advanced thermo–physical model has been applied to the observational data. To better interpret the spectral features above the thermal emission continuum, we compared the ISO observations with laboratory spectra available in the literature. Several laboratory experiments on minerals and meteorites have been performed to complete the analysis and to study the spectral behavior at various grain sizes. A possible spectral similarity with CO carbonaceous chondrites at small grain size is demonstrated.
Published: 2002

20. D2O and HDS in the coma of 67P/Churyumov–Gerasimenko

Author: André Bieler, Jean-Jacques Berthelier, T. C. Owen, B. Fiethe, Martin Rubin, Sébastien Gasc, Thierry Sémon, S. A. Fuselier, Léna Le Roy, Tamas Gombosi, Chia-Yu Tzou, Hans Balsiger, Kathrin Altwegg, J. De Keyser, Ursina Calmonte, Physikalisches Institut [Bern], Universität Bern [Bern], Center for Space and Habitability (CSH), University of Bern, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] (SwRI), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Universität Bern [Bern] (UNIBE), Center for Space and Habitability ( CSH ), HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], and Southwest Research Institute [San Antonio] ( SwRI )
Subjects: 67P/Churyumov-Gerasimenko, Solar System, 010504 meteorology & atmospheric sciences, General Mathematics, Comet, Analytical chemistry, General Physics and Astronomy, Coma (optics), Astrophysics, 01 natural sciences, Ion, Rosetta, 0103 physical sciences, comets, 010303 astronomy & astrophysics, deuterium, 0105 earth and related environmental sciences, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], General Engineering, Articles, solar system, [ PHYS.PHYS.PHYS-AO-PH ] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Deuterium, Yield (chemistry), High mass, High ratio, space exploration
Abstract: The European Rosetta mission has been following comet 67P/Churyumov–Gerasimenko for 2 years, studying the nucleus and coma in great detail. For most of these 2 years the Rosetta Orbiter Sensor for Ion and Neutral Analysis (ROSINA) has analysed the volatile part of the coma. With its high mass resolution and sensitivity it was able to not only detect deuterated water HDO, but also doubly deuterated water, D2O and deuterated hydrogen sulfide HDS. The ratios for [HDO]/[H2O], [D2O]/[HDO] and [HDS]/[H2S] derived from our measurements are (1.05 ± 0.14) × 10−3, (1.80 ± 0.9) × 10−2and (1.2 ± 0.3) × 10−3, respectively. These results yield a very high ratio of 17 for [D2O]/[HDO] relative to [HDO]/[H2O]. Statistically one would expect just 1/4. Such a high value can be explained by cometary water coming unprocessed from the presolar cloud, where water is formed on grains, leading to high deuterium fractionation. The high [HDS]/[H2S] ratio is compatible with upper limits determined in low-mass star-forming regions and also points to a direct correlation of cometary H2S with presolar grain surface chemistry.This article is part of the themed issue ‘Cometary science after Rosetta’.
Published: 2017

21. Volatile and Organic Compositions of Sedimentary Rocks in Yellowknife Bay, Gale Crater, Mars

Author: M. A. Meyer, Mark I. Richardson, Robert C. Anderson, Marisa C. Palucis, Sara Navarro Lopez, Rodney C. Ewing, Sanjeev Gupta, Caroline Freissinet, Edward M. Stolper, James F. Bell, M. A. Ravine, I. G. Mitrofanov, Thomas F. Bristow, Dawn Y. Sumner, Joel A. Hurowitz, Robert M. Haberle, Claire E. Newman, Andrew Steele, Muriel Saccoccio, Leslie Keely, E. Pallier, Jason P. Dworkin, Claude Geffroy, Mary A. Voytek, Michael Caplinger, Fred Goesmann, Yann Parot, Maria-Paz Zorzano Mier, A. B. Sanin, S. W. Squyres, Javier Caride Rodriguez, J. L. Griffes, Julio José Romeral-Planello, Jason Feldman, Katherine L. French, V. Sautter, Nicolas Mangold, David L. Bish, Vivian Lafaille, Michael D. Smith, François Raulin, V. Prokhorov, Gilles Berger, S. Slavney, Heather B. Franz, S. Johnstone, Susanne P. Schwenzer, Felipe Gómez, Harri Haukka, Francis A. Cucinotta, J. Hudgins, T. Cleghorn, Pascaline Francois, Alain Lepinette Malvitte, Shuai Li, Paul R. Mahaffy, K. M. Robertson, Bruce M. Jakosky, J. Guo, Juergen Schieber, Rafael Navarro-González, G. J. Flesch, Scott M. McLennan, Jennifer G. Blank, M. Carmosino, Kenneth A. Farley, Yves Langevin, P. D. Archer, A. E. Brunner, M. D. Dyar, S. Le Mouélic, V. Hipkin, Sara Alejandra Sans Fuentes, Kenneth S. Edgett, Sabrina Feldman, Gale Paulsen, Paul Herrera, Alberto G. Fairén, Kirsten L. Siebach, Jan-Peter Muller, M. J. Schoppers, Eldar Noe Dobrea, Nina Lanza, Marc Gailhanou, Genevieve Marchand, Sönke Burmeister, Craig Hardgrove, Justin N. Maki, Ari-Matti Harri, Michael C. Malin, M. J. Wolff, Roger E. Summons, H. Blau, Jacqueline Cameron, Jeff A. Berger, Didier Keymeulen, Agnes Cousin, Guillermo M. Muñoz Caro, Eric Lyness, Cedric Pilorget, Michael B. Baker, Christopher S. Edwards, M. L. Litvak, Brian M. Duston, Rebecca M. E. Williams, T. Nolan, Robert T. Downs, V. E. Hamilton, Walter Goetz, Pamela G. Conrad, J. Baroukh, Nathan T. Bridges, Meenakshi Wadhwa, Roger C. Wiens, Samuel M. Clegg, Philippe Sarrazin, L. Bleacher, Eric Lorigny, Mike Toplis, Michael H. Wong, Timothy H. McConnochie, Ian Mcewan, Kiran Patel, Mary Beth Wilhelm, John P. Grotzinger, Jeffrey E. Moersch, Michael A. Wilson, Mark Paton, I. Plante, Eric Lewin, Franck Poitrasson, Tori M. Hoehler, P. Guillemot, Mackenzie Day, David F. Blake, José Antonio Rodríguez Manfredi, G. W. Lugmair, Robert F. Wimmer-Schweingruber, Dorothy Z. Oehler, Samuel Teinturier, Bent Ehresmann, Jérémie Lasue, K. E. Herkenhoff, Daniel C. Berman, Scott VanBommel, Jeffrey R. Johnson, Emily M. McCullough, A. A. Fraeman, Ezat Heydari, Penelope L. King, K. M. Stack, Diana L. Blaney, A. Salamon, John G. Spray, L. Posiolova, Jeff Hollingsworth, David Choi, Kevin W. Lewis, B. D. Prats, Tonci Balic-Zunic, Mehdi Benna, H. M. Elliott, Jesús Martínez-Frías, R. Mueller-Mellin, William V. Boynton, Lance E. Christensen, Richard Leveille, John A. Grant, David E. Harker, J. M. Morookian, Caleb I. Fassett, S. Jacob, Donald Fay, R. Perez, Horton E. Newsom, Morten Madsen, M. G. Trainer, G. Israel, B. E. Nixon, Claude d’Uston, John E. Moores, Olivier Gasnault, Daniel J. Krysak, Vladislav Tretyakov, G. M. Perrett, Andrew D. Aubrey, L. E. Kirkland, F. Stalport, B. L. Barraclough, Alain Cros, Stephan Böttcher, Michel Cabane, William B. Brinckerhoff, Jack D. Farmer, James J. Wray, P. Y. Meslin, Arnaud Buch, Allan H. Treiman, S. C. R. Rafkin, B. C. Clark, Noureddine Melikechi, R. Jackson, Luther W. Beegle, Angela Lundberg, Bethany L. Ehlmann, William E. Dietrich, Karl Iagnemma, K. Supulver, Radu Popa, R. Zimdar, Melissa Floyd, Wesley T. Huntress, Paul B. Niles, D. M. Delapp, C. N.. Achilles, Darrell Drake, T. Nelson, Alain Gaboriaud, Verónica Peinado-Gonzalez, Edward P. Vicenzi, T. Boucher, Jennifer L. Eigenbrode, C. Tate, David J. Des Marais, F. Javier Martin-Torres, Antoine Charpentier, Chris Webster, Mildred P. Martin, Robert M. Sucharski, Lucy M. Thompson, Cyril Szopa, D. Halleaux, Antonio Molina Jurado, Richard V. Morris, Andrey Vostrukhin, Peter C. Thomas, Ara V. Nefian, Pablo Sobron Sanchez, Manuel de la Torre Juárez, B. Elliott, Hannu Savijärvi, J. Bentz, Sergey Nikiforov, S. Gordon, Shaunna M. Morrison, Jean-Luc Lacour, Günter Reitz, M. E. Newcombe, David E. Brinza, C. Yana, Gary Kocurek, L. J. Lipkaman, C. M. Garcia, Maria Genzer, Fred Calef, A. Godber, Stubbe F. Hviid, C. Donny, T. Van Beek, Ruslan O. Kuzmin, Alexander Hayes, T. S. Olson, George D. Cody, J. Martín-Soler, N. Karpushkina, John Bridges, Mercedes Jiménez, M. Lefavor, Sylvestre Maurice, H. L. K. Manning, Ralph E. Milliken, Susanne Schröder, N. Spanovich, L. J. Edwards, A. Koefoed, Roser Urqui-O'Callaghan, Eduardo Sebastian Martinez, Cary Zeitlin, Noël Stewart, David T. Vaniman, E. A. Breves, Laurent Favot, A. Varenikov, Gérard Manhès, R. B. Williams, David Martin, Steven J. Rowland, E. Boehm, Adrian P. Jones, Alexis Paillet, R. Francis, Sushil K. Atreya, Mariek E. Schmidt, David Baratoux, N. I. Boyd, Qiu-Mei Lee, I. L. ten Kate, Bernard Hallet, K. Stoiber, Vivian Z. Sun, M. R. Kennedy, Gillian M. Krezoski, Mark A. Bullock, T. Stein, Michelle E. Minitti, I. Pradler, Susan L. S. Stipp, Scott Davis, Robert O. Pepin, B. L. Ehlmann, Janne Kauhanen, Dmitry Golovin, Steve J. Chipera, Raymond E. Arvidson, Javier Gómez-Elvira, L. C. Kah, Melissa S. Rice, Isaias Carrasco Blazquez, Cécile Fabre, John J. Simmonds, Joy A. Crisp, Jens Frydenvang, Florence Tan, Julia DeMarines, S. P. Gorevan, Elizabeth B. Rampe, E. McCartney, Lauren DeFlores, K. Harshman, D. N. Harpold, J. Van Beek, Luis Mora-Sotomayor, Douglas W. Ming, Kristen E. Miller, John Campbell, Amy McAdam, L. Saper, Robert Sullivan, Lorenzo Fluckiger, Kjartan M. Kinch, Arik Posner, H. Bower, A. A. Pavlov, D. Scholes, Insoo Jun, Brigitte Gondet, Patrice Coll, Burt Baker, Donald M. Hassler, Ralf Gellert, Laurie A. Leshin, T. Siili, Gilles Dromart, Lauren A. Edgar, Ryan B. Anderson, Robert Dingler, Leon Radziemski, Jean-Baptiste Sirven, G. Weigle, Cynthia K. Little, A. Mezzacappa, Olivier Forni, A. S. Kozyrev, Edward A. Cloutis, Ashwin Vasavada, A. Behar, François Robert, D. M. Rubin, Alexey Malakhov, E. Jensen, T. C. Owen, Sebastien Hettrich, Miguel Ramos, B. Sutter, Melinda A. Kahre, Patrick Pinet, John H. Jones, Claude Brunet, B. Pavri, Nilton O. Renno, Evgeny Atlaskin, Laurent Peret, Maxim Mokrousov, David Lees, J. J. B. Avalos, Jennifer C. Stern, Ann Ollila, Josefina Torres Redondo, Miles J. Johnson, M. A. D. P. Hernandez, Daniel P. Glavin, Albert S. Yen, Christophe Agard, Jouni Polkko, Christopher P. McKay, J. Peterson, Oliver Botta, Mark T. Lemmon, Marion Nachon, K. M. Bean, Bruce A. Cantor, Jan Köhler, M. Fitzgibbon, Carlos Armiens-Aparicio, Jorge Pla-Garcia, Henrik Kahanpää, Frances Westall, Walter Schmidt, M.-H. Kim, Kenneth G. Miller, Sharon A. Wilson, S. McNair, O. Kortmann, David Grinspoon, E. M. Lee, S. Indyk, Osku Kemppinen, E. Raaen, Michael Mischna, R. S. Sletten, James B. Garvin, John M. Ward, R. L. Tokar, Paulo M. Vasconcelos, Charles Malespin, T. J. Parker, Aaron J. Sengstacken, S. Bender, Jean-Pierre Williams, F. Fedosov, Patrick Mauchien, Audrey Dupont, R. A. Yingst, David Coscia, David A. Cremers, Danika Wellington, Kenneth H. Nealson, J. K. Jensen, Martin R. Fisk, J. Joseph, Amy J. Williams, W. Brunner, NASA Johnson Space Center (JSC), NASA, NASA Goddard Space Flight Center (GSFC), Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Guelph], University of Guelph, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Space Science and Astrobiology Division at Ames, NASA Ames Research Center (ARC), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Astronomy [Ithaca], Cornell University [New York], Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth Science and Technology [Imperial College London], Imperial College London, United States Geological Survey [Reston] (USGS), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Rensselaer Polytechnic Institute (RPI), Princeton University, State University of New York (SUNY), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), NOAA Earth System Research Laboratory (ESRL), National Oceanic and Atmospheric Administration (NOAA), Lunar and Planetary Institute [Houston] (LPI), Planetary Science Institute [Tucson] (PSI), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Aalto University, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Applied Research Associates, Inc. (ARA), Center for Meteorite Studies [Tempe], Ashima Research, ATOS Origin, Australian National University (ANU), Bay Area Environmental Research Institute (BAER), Big Head Endian LLC, Brock University [Canada], Brown University, Canadian Space Agency (CSA), Capgemini Consulting [Paris], Carnegie Mellon University [Pittsburgh] (CMU), Catholic University of America, Institut des Matériaux, de Microélectronique et des Nanosciences de Provence (IM2NP), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Chesapeake Energy Corporation, Service de la Corrosion et du Comportement des Matériaux dans leur Environnement (SCCME), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Interaction Laser Matière (LILM), Concordia College, Moorhead, CS-Systèmes d'Information [Toulouse] (CS-SI), Delaware State University (DSU), Denver Museum of Nature and Science, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Finnish Meteorological Institute (FMI), GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Géosciences Environnement Toulouse (GET), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Global Science and Technology, Inc., Honeybee Robotics Ltd, Indiana University [Bloomington], Indiana University System, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie des Milieux et Matériaux de Poitiers (IC2MP), Université de Poitiers-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Institut des Sciences de la Terre (ISTerre), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Jackson State University (JSU), Jacobs Technology ESCG, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Minéralogie et Cosmochimie du Muséum (LMCM), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Space Remote Sensing Group (ISR-2), Malin Space Science Systems (MSSS), Depertment of Polymer Chemistry, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DLR Institute of Planetary Research, German Aerospace Center (DLR), NASA Headquarters, Oregon State University (OSU), Search for Extraterrestrial Intelligence Institute (SETI), Smithsonian Institution, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), TechSource Inc., Texas A&M University [College Station], The Open University [Milton Keynes] (OU), University of Arizona, Met Office Hadley Centre for Climate Change (MOHC), United Kingdom Met Office [Exeter], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), California Institute of Technology (CALTECH)-NASA, Universidad Nacional Autónoma de México (UNAM), Carnegie Institution for Science [Washington], University of California [Berkeley], University of California-University of California, Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN), and Kruch, Catherine
Subjects: Geologic Sediments, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Curiosity rover, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Sulfides, 01 natural sciences, organic compositions, Bassanite, 0103 physical sciences, Exobiology, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Hydrocarbons, Chlorinated, MSL, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Total organic carbon, Martian, mudstone samples, Volatile Organic Compounds, Multidisciplinary, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Water, Mars Exploration Program, Carbon Dioxide, Oxygen, Bays, 13. Climate action, Rocknest, Sample Analysis at Mars, Sedimentary rock, Pyrolysis
Abstract: H 2 O, CO 2 , SO 2 , O 2 , H 2 , H 2 S, HCl, chlorinated hydrocarbons, NO, and other trace gases were evolved during pyrolysis of two mudstone samples acquired by the Curiosity rover at Yellowknife Bay within Gale crater, Mars. H 2 O/OH-bearing phases included 2:1 phyllosilicate(s), bassanite, akaganeite, and amorphous materials. Thermal decomposition of carbonates and combustion of organic materials are candidate sources for the CO 2 . Concurrent evolution of O 2 and chlorinated hydrocarbons suggests the presence of oxychlorine phase(s). Sulfides are likely sources for sulfur-bearing species. Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the mudstone; however, the carbon source for the chlorinated hydrocarbons is not definitively of martian origin.
Published: 2014

22. Adaptive Optics Observations of Saturn's Ring Plane Crossing in August 1995

Author: T. C. Owen, André Brahic, Francois Roddier, J. E. Graves, Malcolm J. Northcott, Claude Roddier, and Christophe Dumas
Subjects: Physics, Space and Planetary Science, Infrared, Saturn, Rings of Saturn, Resolution (electron density), Astronomy, Astronomy and Astrophysics, Moons of Saturn, Astrophysics, Janus, Ring (chemistry), Adaptive optics
Abstract: Adaptive optics (0.15″ resolution) infrared images of the rings and satellites of Saturn were obtained in August 1995 as the Earth was crossing the ring plane. Twelve clumps were detected in the F ring, including HST S5 and S7 objects. For the first time H magnitudes were obtained for Prometheus, Pandora, Telesto, and Calypso, and J magnitudes for Epimetheus, Janus, Mimas, Telesto, and Helene.
Published: 2000

23. From the Interstellar Medium to Earth's Oceans via Comets—An Isotopic Study of HDO/H2O

Author: T. C. Owen, Akiva Bar-Nun, G. Notesco, and D. Laufer
Subjects: Interstellar medium, Materials science, Space and Planetary Science, Molecular cloud, Astronomy and Astrophysics, Formation and evolution of the Solar System, Water vapor, Earth (classical element), Astrobiology
Abstract: The isotopic enrichment of HDO over H 2 O when water vapor freezes into ice at 60–170 K was studied experimentally. No such enrichment was detected (1.003–1.007 in the 95% confidence interval). Thus HDO cannot be enriched when ice is formed by freezing of water vapor. The very similar D/H ratio in the water of Comets Halley, Hyakutake, and Hale–Bopp (∼3 × 10 −4 ) is 10–20 times larger then the D/H ratio in the solar nebula. Therefore the cometary water had to originate in a giant molecular cloud, where the HDO is enriched by ion–molecule reactions. We cannot determine whether the ice grains which agglomerated into these comets were formed in a ∼50 K warm clump in the giant molecular cloud and settled intact to the solar nebula or sublimated and refroze in the ∼50 K Uranus–Neptune region. The HDO/H 2 O ratio in Earth's oceans suggests that the water was delivered by both comets and rocky material formed in Earth's region of the solar nebula.
Published: 1999

24. Detection of Water Ice on Saturn's Satellite Phoebe

Author: Ted L. Roush, T. C. Owen, C. M. Dalle Ore, C. de Bergh, Thomas R. Geballe, and Dale P. Cruikshank
Subjects: Solar System, Materials science, Space and Planetary Science, Asteroid, Absorption band, Saturn, Astronomy, Astronomy and Astrophysics, Astrophysics, Albedo, Absorption (electromagnetic radiation), Grain size, Spectral line
Abstract: The near-infrared reflectance spectrum of Saturn's satellite Phoebe shows a broad absorption band at 2.0 micrometers and absorption at lambda > 2.2 micrometers, both characteristic of H2O ice. We have successfully modeled the surface of Phoebe with an intimate (granular) mix of H2O ice (3% by weight, grain size 500 micrometers) mixed with fine grains of H2O ice (0.25%) with amorphous carbon (grain size 900 micrometers) as the dominant component. This model reproduces the shape of the measured spectrum and the observed albedo of 0.10 for Phoebe, but it is not unique. The presence of ice establishes Phoebe as an original member of the outer Solar System rather than a renegade asteroid.
Published: 1999

25. Neptune's Cloud Structure and Activity: Ground-Based Monitoring with Adaptive Optics

Author: J. E. Graves, T. C. Owen, Claude Roddier, Francois Roddier, and Malcolm J. Northcott
Subjects: Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Cloud computing, Astrophysics::Cosmology and Extragalactic Astrophysics, H band, law.invention, Telescope, Space and Planetary Science, Neptune, law, Angular resolution, Astrophysics::Earth and Planetary Astrophysics, business, Adaptive optics, Astrophysics::Galaxy Astrophysics
Abstract: Since August 1995, near-infrared images of Neptune have regularly been obtained with the University-of-Hawaii telescope. These images reveal Neptune's cloud structure with an angular resolution reaching 0.12″ in the H band.
Published: 1998

26. The Composition of Centaur 5145 Pholus

Author: John K. Davies, Robert H. Brown, Yvonne J. Pendleton, K. A. Tryka, Dale P. Cruikshank, Max P. Bernstein, James F. Bell, C. M. Dalle Ore, T. C. Owen, Thomas R. Geballe, S. M. White, C. de Bergh, David J. Tholen, Ted L. Roush, and Mary Jane Bartholomew
Subjects: Micrometre, Materials science, Absorption spectroscopy, Meteorite, Space and Planetary Science, Asteroid, Comet, Infrared spectroscopy, Astronomy and Astrophysics, Tholin, Astrophysics, Absorption (chemistry)
Abstract: We present a new spectrum of the Centaur object 5145 Pholus between 1.15 and 2.4 micro meters. We model this, and the previously published (0.4- to 1.0- micrometer) spectrum, using Hapke scattering theory. Seen in absorption are the 2.04- micrometer band of H2O ice and a strong band at 2.27 micrometer, interpreted as frozen methanol and/or a photolytic product of methanol having small molecular weight. The presence of small molecules is indicative of a chemically primitive surface, since heating and other processes remove the light hydrocarbons in favor of macromolecular carbon of the kind found in carbonaceous meteorites. The unusually red slope of Pholus' spectrum is matched by fine grains of a refractory organic solid (tholin). Olivine (which we model with Fo 82) also appears to be present on Pholus. We present a five-component model for the composite spectrum of all spectroscopic and photometric data available for 5145 Pholus and conclude that this is a primitive object which has not yet been substantially processed by solar heat. The properties of Pholus are those of the nucleus of a large comet that has never been active.
Published: 1998

27. Near-Infrared Spectroscopy of Low-Albedo Surfaces of the Solar System: Search for the Spectral Signature of Dark Material

Author: T. C. Owen, Christophe Dumas, and M. A. Barucci
Subjects: Physics, education.field_of_study, Solar System, Spectral signature, Infrared, Population, Near-infrared spectroscopy, Astronomy, Astronomy and Astrophysics, Space and Planetary Science, Asteroid, Thermal infrared spectroscopy, education, Spectroscopy
Abstract: We obtained I–J–H–K band spectroscopy of 18 low-albedo objects of the Solar System using the University of Hawaii 88-in. telescope equipped with the near-infrared spectrograph KSPEC. Most of our targets were selected from among the population of the Cybele, Hilda, and Trojan groups of asteroids, based on their low albedos and the relatively steep slopes of their reflection spectra at visible wavelengths. The outer jovian satellite Himalia and the Apollo object 3200 Phaethon were also observed. None of the spectra show absorptions similar to those found in the spectrum of 5145 Pholus, which remains the only asteroid-like object whose H–K band reflection spectrum contains a few broad absorptions due to organics. The near-infrared slope and the (1.0- to 2.2-μm) infrared color-index have been derived for each surface. This sample of primitive objects of the Solar System can be interpreted in terms of cometary-like objects that have undergone different degrees of aging.
Published: 1998

28. Millimeter and Submillimeter Heterodyne Observations of Titan: The Vertical Profile of Carbon Monoxide in Its Stratosphere

Author: Henry E. Matthews, Bruno Bézard, Gabriel Paubert, A. Marten, Daniel Gautier, T. C. Owen, and Taufik Hidayat
Subjects: Physics, Rotational transition, Astronomy and Astrophysics, Astrophysics, Atmospheric sciences, law.invention, Telescope, chemistry.chemical_compound, symbols.namesake, chemistry, Space and Planetary Science, law, Mixing ratio, symbols, Millimeter, Spectral resolution, Titan (rocket family), Stratosphere, Carbon monoxide
Abstract: Millimeter and submillimeter heterodyne observations performed with the IRAM 30-m telescope (Pico Veleta, Spain) and the JCMT (Mauna Kea, Hawaii) have been used to derive the stratospheric distribution of carbon monoxide on Titan. Rotational transition lines from 12 CO J (0 → 1), J (1 → 2), J (2 → 3) at 115.271, 230.538, 345.796 GHz, respectively, as well as the J (1 → 2) and J (2 → 3) lines of the 13 CO isotope at 220.399 and 330.588 GHz, respectively, were recorded with a spectral resolution of 1 MHz. Flux calibration uncertainties were estimated to 10% for all the data. A terrestrial value of the 12 C/ 13 C ratio has been assumed in the analysis as suggested by T. Hidayat et al . (1997, Icarus 126, 170–182) from recent observations of the H 12 CN(1–0) and H 13 CN(4–3) lines. The 13 CO lines sound the 60- to 180-km altitude range, while the 12 CO lines permit us to probe the atmosphere up to an altitude of about 350 km. Below 180 km, the 13 CO data impose a constant-with-height CO mixing ratio of ∼2.5 × 10 −5 . Extending this uniform mixing ratio profile throughout the stratosphere, all the 12 CO observations could be matched only if the systematic calibration errors were greater than our estimated value by at least a factor of 2. Uncertainties related to the temperature profile adopted in the stratosphere have been also investigated. Taking into account random and systematic uncertainties, the entire set of data indicates a CO mixing ratio equal to 2.9 +0.9 −0.5 × 10 −5 at 60 km, decreasing to 2.4 ± 0.5 × 10 −5 at 175 km, and reaching a value of 4.8 +3.8 −1.5 × 10 −6 at 350 km.
Published: 1998

29. Deuterated Water in Comet C/1996 B2 (Hyakutake) and Its Implications for the Origin of Comets

Author: Jocelyn Keene, Jacques Crovisier, Paul F. Goldsmith, Dariusz C. Lis, Dominique Bockelée-Morvan, Thomas G. Phillips, Edwin A. Bergin, Alwyn Wootten, D. Gautier, Didier Despois, T. C. Owen, and K. Young
Subjects: Physics, Caltech Submillimeter Observatory, Deuterium, Space and Planetary Science, Comet, Mass spectrum, Rotational transition, Astronomy and Astrophysics, Astrophysics, Formation and evolution of the Solar System, Planetary nebula, Spectral line
Abstract: The close approach to the Earth of comet C/1996 B2 (Hyakutake) in March 1996 allowed searches for minor volatile species outgassing from the nucleus. We report the detection of deuterated water (HDO) through its 1(sub 01)-0(sub 00) rotational transition at 464.925 GHz using the Caltech Submillimeter Observatory. We also present negative results of a sensitive research for the J(5-4) line of deuterated hydrogen cyanide (DCN) at 362.046 GHz. Simultaneous observations of two rotational lines of methanol together with HDO in the same spectrum allow us to determine the average gas temperature within the telescope beam to be 69 +/- 10 K. We are thus able to constrain the excitation conditions in the inner coma and determine reliably the HDO production rate as (1.20 +/- 0.28) x 10(exp 26)/s on March 23-24, 1996. Available IR, UV and radio measurements lead to a water production rate of (2.1 +/- 0.5) x 10(exp 29)/s at the time of our HDO observations. The resulting D/H ratio in cometary water is thus (29 +/- 10) x 10(exp -5) in good agreement with the values of (30.8(sub - 5.3, sup +3.8) (Balsiger et al. 1995) and (31.6 +/- 3.4) x 10(exp -5) (Eberhardt et al. 1995) determined in comet P/Halley from in situ ion mass spectra. The inferred 3 a upper limit for the D/H ratio in HCN is 1%. Deuterium abundance is a key parameter for studying the origin and the early evolution of the Solar System and of its individual bodies. Our HDO measurement confirms that, in cometary water, deuterium is enriched by a factor of at least 10 relative to the protosolar ratio, namely the D/H ratio in H2 in the primitive Solar Nebula which formed from the collapse of the protosolar cloud. This indicates that cometary water has preserved a major part of the high D/H ratio acquired in this protosolar cloud through ion-molecule isotopic exchanges or grain-surface reactions and was not re-equilibrated with H2 in the Solar Nebula. Scenarios of formation of comets consistent with these results are discussed.
Published: 1998

30. In-Situ Chemical and Isotopic Measurements of the Atmosphere of Jupiter

Author: Hasso B. Niemann, Paul R. Mahaffy, S. K. Atreya, and T. C. Owen
Subjects: Atmosphere, Neon, Materials science, Argon, Xenon, chemistry, Atmosphere of Jupiter, Krypton, Analytical chemistry, Galileo Probe, chemistry.chemical_element, Atmospheric sciences, Helium
Abstract: Insights into both the detailed composition of Jupiter’s atmosphere and unexpected local meteorological phenomena were revealed by in-situ measurements from the Galileo Probe Neutral Mass Spectrometer taken on December 7, 1995. Measurements of the neutral atmospheric composition from a pressure of 0.5 bar to approximately 21 bar revealed the mixing ratios of the major species helium and hydrogen as well as numerous minor constituents including methane, water, ammonia, ethane, ethylene, propane, hydrogen sulfide, neon, argon, krypton, and xenon. This instrument measured the isotope ratios3He/4He, D/H, and13C/12C as well as the isotopes of neon, argon, krypton, and xenon. A summary is given of progress that has been made in refining preliminary estimates of the abundances of condensable volatiles and noble gases as a result of an ongoing laboratory study using a nearly identical engineering unit. The depletion of simple condensable species to depths well below their expected condensation levels is explained by a local downdraft in the region of the probe entry. The mass spectrometer data suggests that different species may recover at different depths and this may be due to lateral mixing of Jovian air.
Published: 1998

31. Millimeter and Submillimeter Heterodyne Observations of Titan: Retrieval of the Vertical Profile of HCN and the12C/13C Ratio☆

Author: Taufik Hidayat, Daniel Gautier, T. C. Owen, Bruno Bézard, Henry E. Matthews, A. Marten, and Gabriel Paubert
Subjects: ICARUS, Physics, Heterodyne, Astronomy and Astrophysics, Astrophysics, Spectral line, symbols.namesake, Altitude, Space and Planetary Science, symbols, Millimeter, Titan (rocket family), Stratosphere, Line (formation), Remote sensing
Abstract: We report new observations of the (1–0) line of HCN at 88.63 GHz, emitted by Titan, made in May 1995 with the IRAM 30-m radiotelescope located at Pico Veleta (Spain). Compared to previous observations of Tanguy et al. (1990, Icarus 85, 43–57), the signal-to-noise ratio has been improved by a factor of 5, permitting us to retrieve the vertical distribution of HCN in the 80–350 km altitude range. Using the production rate of HCN predicted from photochemical models, we derive a profile of the eddy diffusion coefficient up to 350 km altitude consistent with the observed HCN vertical distribution. This coefficient increases with height more rapidly than the standard n −0.5 dependence in the stratosphere. The (4–3) line of H 13 CN at 345.34 GHz was subsequently observed with the JCMT on Mauna Kea (Hawaii) in June 1995. The analysis of the two spectra yields a 12 C/ 13 C ratio between 70 and 120, consistent with the terrestrial value. Taking into account possible fractionation processes, we show that the C-bearing species which formed Titan should have had a carbon isotopic ratio in the same range.
Published: 1997

32. Dark matter in the outer solar system

Author: Dale P. Cruikshank, C. de Bergh, T. C. Owen, and Thomas R. Geballe
Subjects: Physics, Atmospheric Science, Solar System, Planetesimal, Infrared astronomy, Spectroscopy, Near-Infrared, Extraterrestrial Environment, Absorption spectroscopy, Astronomy, Dark matter, Aerospace Engineering, Astronomy and Astrophysics, Meteoroids, Astrophysics, Spectral line, Minor Planets, Saturn, Geophysics, Space and Planetary Science, Exobiology, General Earth and Planetary Sciences, Protoplanet, Absorption (electromagnetic radiation)
Abstract: There are now a large number of small bodies in the outer solar system that are known to be covered with dark material. Attempts to identify that material have been thwarted by the absence of discrete absorption features in the reflection spectra of these planetesimals. An absorption at 2.2 micrometers that appeared to be present in several objects has not been confirmed by new observations. Three absorptions in the spectrum of the unusually red planetesimal 5145 Pholus are well-established, but their identity remains a mystery.
Published: 1995

33. Near-Infrared Spectroscopy of Dark Asteroids

Author: M. A. Barucci, M. Fulchignoni, T. C. Owen, M. Lazzarin, and Cesare Barbieri
Subjects: Physics, ORGANIC MATERIALS, Spectroscopy, Near-Infrared, Extraterrestrial Environment, Absorption spectroscopy, Astronomy, Near-infrared spectroscopy, Infrared spectroscopy, INFRARED SPECTROSCOPY, Astronomy and Astrophysics, Carbon, Spectral line, Minor Planets, law.invention, Telescope, Space and Planetary Science, Observatory, law, Asteroid, Solar System, Evolution, Planetary, Spectrograph
Abstract: Near-infrared (J, H and K bands) spectra of nine dark asteroids (chosen among a sample of supposed primitive objects between C and D classes) have been obtained at the Mauna Kea Observatory (Hawaii) with the 2.2-m telescope using KSPEC as spectrograph. The aim of this work was to search for evidence of the presence of organic materials in these objects as found in other planetary bodies as 5145 Pholus, and in some cometary nuclei. A careful analysis of the data has revealed flat or slightly redder spectra than the solar one for all observed asteroids. No evidence of distinct absorption features was found.
Published: 1994

34. Localization and surgical management of insulinoma

Author: R. C. N. Williamson, M. P. N. Lewis, J. G. Geoghegan, S.R. Bloom, E. R. T. C. Owen, J. A. Lynn, and James E. Jackson
Subjects: Adult, Male, medicine.medical_specialty, Pancreatic disease, Adolescent, endocrine system diseases, Visceral angiography, medicine, Humans, Islet cell hyperplasia, Pancreatic resection, Pancreas, Insulinoma, Aged, Retrospective Studies, medicine.diagnostic_test, business.industry, Middle Aged, medicine.disease, Surgery, Pancreatic Neoplasms, Radiography, Treatment Outcome, Angiography, Female, Ultrasonography, business, Distal pancreatectomy, Splenic Artery, Follow-Up Studies
Abstract: Over a 14-year period 34 patients were referred for surgical treatment of insulinoma. The diagnosis was confirmed by demonstrating hypoglycaemia with inappropriate hyperinsulinaemia during prolonged fasting. Selective visceral angiography localized 30 solitary benign insulinomas and two carcinomas. In two patients with islet cell hyperplasia, angiography demonstrated a single lesion only. Ultrasonography had a sensitivity of 15 per cent and computed tomography a sensitivity of 24 per cent in the localization of tumours. All patients but one were treated by operation. Eighteen tumours were enucleated and 13 (including both patients with islet cell hyperplasia) were treated by distal pancreatectomy. Two patients underwent negative primary exploration; both had single adenomas removed at reexploration. There were no operative deaths but nine patients (predominantly those undergoing pancreatic resection) had complications. Thirty-one patients were symptom-free following operation at a mean follow-up of 16 months.
Published: 1994

35. The use of a water-soluble formazan complex to quantitate the cell number and mitochondrial function ofLeishmania major promastigotes

Author: T C Owen, L Zhai, A Kharazmi, M Chen, and K Berg
Subjects: Time Factors, Tetrazolium Salts, Microbiology, chemistry.chemical_compound, Bromide, Animals, Leishmania major, Pentamidine, Formazans, General Veterinary, biology, Temperature, Substrate (chemistry), General Medicine, Cell counting, biology.organism_classification, Mitochondria, Thiazoles, Infectious Diseases, chemistry, Biochemistry, Parasitology, Antimony Sodium Gluconate, Cell culture, Insect Science, Formazan, Thymidine
Abstract: One of the methods to quantitate Leishmania major promastigotes (LmP) has been to utilize the formation of a formazan dye, which in turn is produced via conversion of an artificial substrate, 3-(4,5-dimethylthiazol-2-yl)-2,5-diphenyltetrazolium bromide (MTT). The method has one major drawback in that the formazan complex precipitates inside the parasites and has to be extracted by denaturants before measurements can be performed. By using a new synthetic substrate, 3-(4,5-dimethylthiazol-2-yl)-5- (3-carboxymethoxyphenyl)-2-(4-sulfonyl)-2H-tetrazolium (MTS), the extraction procedure is eliminated as the formazan-like dye is released spontaneously into the medium, making it possible to perform several measurements on the same parasite culture without disturbing or killing the parasites. The measurements were shown to reflect the numbers of parasites as confirmed via comparative experiments using radioactive thymidine uptake and cell counting, respectively. The method is simple, fast, and highly reproducible and is suitable for drug screening, identification of drug-resistant isolates, and growth-kinetics studies. It is therefore contemplated that the MTS method will be a general and useful technique in this field of parasitology.
Published: 1994

36. The 1.95–2.50 μm Spectrum of J6 Himalia

Author: Dale P. Cruikshank, C. M. Dalle Ore, Thomas R. Geballe, and T. C. Owen
Subjects: Jupiter, Wavelength, Materials science, Optics, Space and Planetary Science, business.industry, Analytical chemistry, Astronomy and Astrophysics, Spectral resolution, Spectroscopy, business, Reflectivity
Abstract: The reflectance spectrum of Jupiter's sixth satellite, Himalia, is featureless in the wavelength region 1.95–2.50 μm as seen at a spectral resolution of 0.005 μm, with no absorptions deeper than a few percent. From model calculations we establish an upper limit of 10% by weight of H 2 O (30-μm grains) mixed intimately in the soil of Himalia, or alternatively 0.3% of the surface covered by exposures of H 2 O ice spatially segregated from the darker soil. For CH 4 and CO 2 ices the upper limits in spatially segregated models are both 0.3%.
Published: 2002

37. ChemInform Abstract: 2-Acetyl-3-methylbenzothiazolium Trifluoromethanesulfonate and Its Rearrangement into 2-Hydroxy-2,4-dimethyl-2H-1,4-benzothiazin-3(4H)- one

Author: G. J. S. Doad and T. C. Owen
Subjects: Chemistry, Organic chemistry, General Medicine, Trifluoromethanesulfonate
Published: 2010

38. Working Group on Planetary System Nomenclature (Wgpsn): (Groupe de Travail Pour la Nomenclature du Systeme Planetaire)

Author: K. Aksnes, M. E. Davies, C. de Bergh, M. Ya. Marov, B.G. Marsden, P. Moore, T. C. Owen, V. V. Shevchenko, B. A. Smith, J. Blue, G. A. Burba, L. Gaddis, and P. Masson
Subjects: Committee on Space Research, History, General assembly, Asteroid, Astronomy, Nomenclature
Abstract: Since July 1996, 815 new names on features on bodies in the Solar System have been assigned by the WGPSN and approved at the IAU General Assembly in Kyoto in 1997. Of these names, 666 were for Venus, 17 for Mars, 3 for the Moon, 125 for the Galilean satellites, 3 for the Uranian satellite Miranda, and 1 for the minor planet Ida. 71 additional names mostly on Venus have been selected and have been given or are awaiting provisional approval by the IAU Executive Committee (EC). These names are up for final approval at the next IAU General Assembly.
Published: 2000

39. Origin and Early Evolution of Comet Nuclei

Author: T. C. Owen, Rita Schulz, W. F. Huebner, Kathrin Altwegg, and Hans Balsiger
Subjects: Physics, Astrophysics and Astronomy, Comet dust, Comet, Astronomy, law.invention, Astrobiology, Orbiter, Planetary science, law, Planet, Comet nucleus, Interstellar comet, Amorphous ice
Abstract: Foreword.- Origins of Cometary Materials.- Origin of Comet Nuclei and Dynamics.- Reservoir for Comet Material: Circumstellar Grains.- Interstellar Reservoirs of Cometary Matter.- Cometary Refractory Grains: Interstellar and Nebular Sources.- Dynamical Origin of Comets and Their Reservoirs.- Reservoirs for Comets: Compositional Differences Based on Infrared Observations.- Thermal and Chemical Evolution of Comet Nuclei and Kuiper Belt Objects.- Loss of the Surface Layers of Comet Nuclei.- Distributed Sources in Comets.- How Well Do Experimental Results on Large Samples of Gas-Laden Amorphous Ice Duplicate Deep Impact's Findings?.- Comet Knudsen Layers.- Morphology-Composition-Isotopes: Recent Results from Observations.- Deep Impact and the Origin and Evolution of Cometary Nuclei.- Assessing the elemental composition of comet 81P/Wild 2 by analyzing dust collected by Stardust.- Composition Measurements of a Comet from the Rosetta Orbiter Spacecraft.- Capabilities of Philae, the Rosetta Lander.- Rapporteur Paper on the Composition of Comets.- The Contributions of Comets to Planets, Atmospheres, and Life: Insights from Cassini-Huygens, Galileo, Giotto, and Inner Planet Missions.
Published: 2008

40. Exploring the Saturn System in the Thermal Infrared: The Composite Infrared Spectrometer

Author: F. M. Flasar, V. G. Kunde, M. M. Abbas, R. K. Achterberg, P. Ade, A. Barucci, B. Bézard, G. L. Bjoraker, J. C. Brasunas, S. Calcutt, R. Carlson, C. J. Césarsky, B.J. Conrath, A. Coradini, R. Courtin, A. Coustenis, S. Edberg, S. Edgington, C. Ferrari, T. Fouchet, D. Gautier, P. J. Gierasch, K. Grossman, P. Irwin, D. E. Jennings, E. Lellouch, A. A. Mamoutkine, A. Marten, J. P. Meyer, C. A. Nixon, G. S. Orton, T. C. Owen, J. C. Pearl, R. Prangé, F. Raulin, P. L. Read, P. N. Romani, R. E. Samuelson, M. E. Segura, M. R. Showalter, A. A. Simon-Miller, M. D. Smith, J. R. Spencer, L. J. Spilker, and F. W. Taylor
Published: 2005

41. Improved constraints on Neptune's atmosphere from submillimetre-wavelength observations

Author: Taufik Hidayat, A. Marten, R. Moreno, Henry E. Matthews, T. C. Owen, Y. Biraud, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Joint Astronomy Centre (JAC), Institute for Astronomy, University of Hawaii, and Department of Astronomy and Bosscha Observatory
Subjects: Physics, Atmosphere, Solar System, Wavelength, Mauna kea, Space and Planetary Science, Neptune, Rotational transition, Astronomy, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], James Clerk Maxwell Telescope
Abstract: International audience; We describe observations of Neptune carried out using the James Clerk Maxwell Telescope (Mauna Kea, Hawaii) during September 1998. High-quality data for the sub-mm-wavelength rotational transitions of HCN (J=4-3) and CO (J=3-2 and 4-3) were obtained, and we use the data to make improved determinations of the abundances of these trace species and the temperature profile of Neptune's atmosphere.
Published: 2005

42. Astrobiology: Future Perspectives

Author: D. Despois, Pascale Ehrenfreund, Anne Dutrey, François Robert, Luigi Colangeli, T. C. Owen, Antonio Lazcano, John Robert Brucato, William M. Irvine, Jen Blank, Sylvie Derenne, and Luann Becker
Subjects: Interstellar medium, chemistry.chemical_classification, Astrophysics and Astronomy, Solar System, Interplanetary dust cloud, Chondrite, Planet, Chemistry, Abiogenesis, Biosignature, Organic matter, Astrobiology
Abstract: Preface. 1 The Synthesis of the Elements and the Formation of Stars M. Spaans. 2 Organic Molecules in the Interstellar Medium T.J. Millar. 3 Chemistry of Protoplanetary Disks Relation to Primitive Solar System Material A.J. Markwick and S.B. Charnley. 4 Planet Formation: Problems and Prospects G. Wuchterl. 5 From Elemental Carbon to Complex Macromolecular Networks in Space F. Cataldo. 6 Organic Molecules in Planetary Atmospheres M. Roos-Serote. 7 Observations and Laboratory Data of Planetary Organics T.L. Rousch and D.P. Cruikshank. 8 The Molecular Complexity of Comets J. Crovisier. 9 Kuiper belt: Water and Organics C. de Bergh. 10 Interplanetary Dust Particles and Astrobiology F.J. Molster. 11 The Prebiotic Atmosphere of the Earth F. Selsis. 12 Early Life on Earth: The Ancient Fossil Record F. Westall. 13 Highly Altered Organic Matter on Earth: Biosignature Relevance B.A. Hofmann. 14 Insoluble Organic Matter in Carbonaceous Chondrites and Archean Cherts. An Insight into their Structure by Electron Paramagnetic Resonance L. Binet, D. Gourier, A. Skrzypczak, S. Derenne, and F. Robert. 15 The Chemistry of the Origin of Life O. Botta. 16 A Novel Synthesis of Biomolecular Precursors R. Saladino, C. Creestini, F. Ciciriello, G. Costanzo, R. Negri, and E. Di Mauro.
Published: 2005

43. The Outer Planets and their Moons

Author: Thérèse Encrenaz, T. C. Owen, R. Kallenbach, and Christophe Sotin
Subjects: Physics, Astrophysics and Astronomy, Solar System, Outer planets, 010304 chemical physics, 13. Climate action, Physics::Space Physics, 0103 physical sciences, Astronomy, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Astrobiology
Abstract: This volume gives an integrated summary of the science related to the four giant planets in our solar system. It is the result of an ISSI workshop on «A comparative study of the outer planets before the exploration of Saturn by Cassini-Huygens» which was held at ISSI in Bern on January 12-16, 2004. Representatives of several scientific communities, such as planetary scientists, astronomers, space physicists, chemists and astrobiologists have met with the aim to review the knowledge on four major themes: (1) the study of the formation and evolution processes of the outer planets and their satellites, beginning with the formation of compounds and planetesimals in the solar nebula, and the subsequent evolution of the interiors of the outer planets, (2) a comparative study of the atmospheres of the outer planets and Titan, (3) the study of the planetary magnetospheres and their interactions with the solar wind, and (4) the formation and properties of satellites and rings, including their interiors, surfaces, and their interaction with the solar wind and the magnetospheres of the outer planets. Beyond these topics, the implications for the prebiotic chemical evolution on Europa and Titan are reviewed. The volume is intended to provide active researchers in the fields of planetary and solar system science, space plasma physics, and astrobiology with an up-to-date status report on the topic, and also to serve graduate students with introductory material into the field. At the time of publication of this book, the study of the outer planets is particularly motivated by the fact that the Saturn system is being investigated by the Cassini-Huygens mission. Reprinted from Space Science Reviews, Volume 116, Nos. 1-2, 2005
Published: 2005

44. Jupiter's atmospheric composition from the Cassini thermal infrared spectroscopy experiment

Author: Bruno Bézard, Paul N. Romani, Amy A. Simon-Miller, R. K. Achterberg, Peter J. Gierasch, Mian M. Abbas, Y. Biraud, Chiara Ferrari, Robert E. Samuelson, Peter L. Read, D. E. Jennings, A. Marten, Peter A. R. Ade, Angioletta Coradini, Athena Coustenis, Regis Courtin, François Raulin, A. A. Mamoutkine, Linda Spilker, T. C. Owen, Gordon L. Bjoraker, John C. Pearl, Darrell F. Strobel, K. Grossman, M. D. Smith, Patrick G. J. Irwin, Conor A. Nixon, Ronald Carlson, Thierry Fouchet, Fredric W. Taylor, P. Parrish, Antonella Barucci, Emmanuel Lellouch, R. Prangé, John C. Brasunas, C. J. Cesarsky, Barney J. Conrath, F. M. Flasar, S. B. Calcutt, Daniel Gautier, V. G. Kunde, Glenn S. Orton, Department of Astronomy, University of Maryland, NASA/Goddard Space Flight Center (NASA/GSFC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Earth and Planetary Sciences, Johns Hopkins University, Department of Astronomy, Cornell University, Space Science and Applications, Atmospheric, Oceanic and Planetary Physics, Department of Physics, Clarendon Laboratory, University of Oxford, Jet Propulsion Laboratory, California Institute of Technology (JPL), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institute for Astronomy, University of Hawaii, Marshall Space Flight Center, NASA, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Cardiff University, European Southern Observatory (ESO), Department of Physics, Gesamthochschule Wuppertal, Instituto di Astrofisica Spaziale - CNR, Area della recerca di Tor Vergata, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), and School of Physics and Astronomy, Cardiff University
Subjects: Ethane, Multidisciplinary, Extraterrestrial Environment, Chemistry, Infrared, Acetylene, Atmosphere, Spectrum Analysis, Comet, Temperature, Methyl radical, Infrared spectroscopy, Hot spot (veterinary medicine), Carbon Dioxide, Hydrocarbons, Astrobiology, Jupiter, chemistry.chemical_compound, Thermal infrared spectroscopy, Hydrogen Cyanide, Spacecraft, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; The Composite Infrared Spectrometer observed Jupiter in the thermal infrared during the swing-by of the Cassini spacecraft. Results include the detection of two new stratospheric species, the methyl radical and diacetylene, gaseous species present in the north and south auroral infrared hot spots; determination of the variations with latitude of acetylene and ethane, the latter a tracer of atmospheric motion; observations of unexpected spatial distributions of carbon dioxide and hydrogen cyanide, both considered to be products of comet Shoemaker-Levy 9 impacts; characterization of the morphology of the auroral infrared hot spot acetylene emission; and a new evaluation of the energetics of the northern auroral infrared hot spot.
Published: 2004

45. 9969 Braille: Deep Space 1 infrared spectroscopy, geometric albedo, and classification

Author: S. A. Stern, Andrew S. Rivkin, R. H. Brown, T. C. Owen, Roland Meier, Bill R. Sandel, Juergen Oberst, Michael D. Hicks, Daniel T. Britt, Roger V. Yelle, Daniel C. Boice, Bonnie J. Buratti, Nicolas Thomas, L. A. Soderblom, and Robert M. Nelson
Subjects: Physics, 9969 Braille, business.industry, Astronomy and Astrophysics, Astrophysics, Albedo, Braille, Spectral line, Asteroids, Optics, NEOs, Meteorite, Space and Planetary Science, Chondrite, Absorption band, Geometric albedo, Asteroid, Deep Space 1, business
Abstract: Spectra of Asteroid 9969 Braille in the 1.25–2.6 µm region returned by the Deep Space 1 (DS1) Mission show a ∼ 10% absorption band centered at 2 µm, and a reflectance peak at 1.6 µm. Analysis of these features suggest that the composition of Braille is roughly equal parts pyroxene and olivine. Its spectrum between 0.4 and 2.5 µm suggests that it is most closely related to the Q taxonomic type of asteroid. The spectrum also closely matches that of the ordinary chondrites, the most common type of terrestrial meteorite. The geometric albedo of Braille is unusually high (pv = 0.34), which is also consistent with its placement within the rarer classes of stony asteroids, and which suggests it has a relatively fresh, unweathered surface, perhaps due to a recent collision.
Published: 2004

46. Future Perspectives and Strategies in Astrobiology

Author: John Robert Brucato, Luann Becker, Jennifer G. Blank, Antonio Lazcano, Bill Irvine, Luigi Colangeli, François Robert, T. C. Owen, D. Despois, Pascale Ehrenfreund, Anne Dutrey, and Sylvie Derenne
Subjects: Planetary science, Future perspective, Geography, Documentation, Relevance (information retrieval), Subject (documents), Astrobiology
Abstract: The subject of Astrobiology can be approached from many different perspectives, as reflected in numerous textbooks, journals, conference proceedings, web documentation and popular literature. This book is focused on abiotic organic matter from the viewpoint of astronomy and planetary science and considers its potential relevance to the origins of life on Earth and elsewhere. Guided by the review papers in this book, this concluding chapter aims to identify key questions to motivate future research and stimulate astrobiological applications of current and future research facilities and space missions.
Published: 2004

47. A 0.4-2.5 μm spectroscopic investigation of Triton's two faces

Author: Cesare Barbieri, Enrico Maria Corsini, Simone Marchi, Monica Lazzarin, and T. C. Owen
Subjects: planetary satellites, spectroscopy, Materials science, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Natural satellite, New Technology Telescope, Spectroscopy, Spectral line
Abstract: We have obtained new observations of Triton with the ESO New Technology Telescope (La Silla, Chile) in October 2002. Using the high quality of NTT instrumentation, we were able to cover the entire 0.4–2.5 μm spectral range in a single night. We applied this procedure for two nights, well selected along the orbit of Triton, in order to cover essentially the trailing side one night, and the leading one the other night, obtaining the first face-resolved 0.4–2.4 μm spectra of Triton. We discuss here the spectra and the differences between the two faces, and the implications of these new results for a better understanding of the surface composition of Triton. In particular we found possible clues for the presence of rocky materials on Triton's surface.
Published: 2004

48. Solar System History from Isotopic Signatures of Volatile Elements

Author: R. Kallenbach, K. Mauersberger, Th. Encrenaz, Johannes Geiss, François Robert, and T. C. Owen
Subjects: Physics, Solar System, Earth science, Volatiles, Astrobiology
Published: 2003

49. Aviation Employment in the US: A Review of Data Sources

Author: David A. NewMyer and Russell T. C. Owen
Subjects: Telephone survey, Finance, Government, Scope (project management), business.industry, Aviation, Terrorism, Aerospace manufacturing, Aerospace, business, Education
Abstract: The aviation industry—particularly the airline and aviation/aerospace manufacturing segments— has received significant negative attention due to financial and employment losses that it has suffered since the terrorist attacks of September 11, 2001. For example, nearly 150,000 jobs have been reported cut at the airlines and aviation/aerospace manufacturers combined. However, there is little said about the overall aviation industry backdrop for these cuts: How large is US aviation industry employment after these publicly announced cuts? The problem addressed by this research was one of finding sources to determine the overall size and scope of aviation industry employment in the US. A literature review was used that examined government documents, scholarly journals, aviation industry journals and information provided by aviation industry associations. In addition, the results of a telephone survey of the top 100 airline-served airports in the US were utilized. The literature review found that US aviation industry employment as of 2002 ranged from 1,870,400 to 2,169,845 depending on the data sources used to arrive at the total. It was also concluded that there are data details not available from the US Department of Labor employment statistics on the aviation industry that are important to determining a conclusive aviation industry employment estimate.
Published: 2003

50. Contributions of icy planetesimals to the Earth's early atmosphere

Author: T C, Owen and A, Bar-Nun
Subjects: Extraterrestrial Environment, Earth, Planet, Nitrogen, Ice, Temperature, Mars, Neon, Gases, Meteoroids, Solar System, Evolution, Planetary, Noble Gases, Venus
Abstract: Laboratory experiments on the trapping of gases by ice forming at low temperatures implicate comets as major carriers of the heavy noble gases to the inner planets. These icy planetesimals may also have brought the nitrogen compounds that ultimately produced atmospheric N2. However, if the sample of three comets analyzed so far is typical, the Earth's oceans cannot have been produced by comets alone, they require an additional source of water with low D/H. The highly fractionated neon in the Earth's atmosphere may also indicate the importance of non-icy carriers of volatiles. The most important additional carrier is probably the rocky material comprising the bulk of the mass of these planets. Venus may require a contribution from icy planetesimals formed at the low temperatures characteristic of the Kuiper Belt.
Published: 2001

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