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1. 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

2. 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

3. 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

4. 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

5. 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

6. 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

7. 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

8. 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

9. 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

10. 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

11. 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

12. 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

13. 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

14. 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

15. 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

16. 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

17. 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

18. 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

19. 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

20. 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

21. 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

22. 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

23. The composition of the Jovian atmosphere as determined by the Galileo probe mass spectrometer

Author: G. R. Carignan, T. C. Owen, Wayne Kasprzak, Donald M. Hunten, Richard E. Hartle, J. A. Haberman, Paul R. Mahaffy, D. N. Harpold, S. H. Way, Sushil K. Atreya, T. M. Donahue, and H. B. Niemann
Subjects: Atmospheric Science, Planetesimal, Materials science, Extraterrestrial Environment, Analytical chemistry, Galileo Probe, Soil Science, Aquatic Science, Oceanography, Mass spectrometry, Helium, Noble Gases, Jovian, Mass Spectrometry, Atmosphere, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Mixing ratio, Spacecraft, Mixing (physics), Earth-Surface Processes, Water Science and Technology, Ecology, Paleontology, Astronomy, Forestry, Space Flight, Galaxy, Carbon, Hydrocarbons, Geophysics, Space and Planetary Science, Jupiter, Calibration, Gases, Hydrogen
Abstract: The Galileo probe mass spectrometer determined the composition of the Jovian atmosphere for species with masses between 2 and 150 amu from 0.5 to 21.1 bars. This paper presents the results of analysis of some of the constituents detected: H2, He, Ne, Ar, Kr, Xe, CH4, NH3, H2O, H2S, C2 and C3 nonmethane hydrocarbons, and possibly PH3 and Cl. 4He/H2 in the Jovian atmosphere was measured to be 0.157 +/- 0.030. 13C/C12 was found to be 0.0108 +/- 0.0005, and D/H and 3He/4He were measured. Ne was depleted,or = 0.13 times solar, Aror = 1.7 solar, Kror = 5 solar, and Xeor = 5 solar. CH4 has a constant mixing ratio of (2.1 +/- 0.4) x 10(-3) (12C, 2.9 solar), where the mixing ratio is relative to H2. Upper limits to the H2O mixing ratio rose from 8 x 10(-7) at pressures3.8 bars to (5.6 +/- 2.5) x 10(-5) (16O, 0.033 +/- 0.015 solar) at 11.7 bars and, provisionally, about an order of magnitude larger at 18.7 bars. The mixing ratio of H2S was10(-6) at pressures less than 3.8 bars but rose from about 0.7 x 10(-5) at 8.7 bars to about 7.7 x 10(-5) (32S, 2.5 solar) above 15 bars. Only very large upper limits to the NH3 mixing ratio have been set at present. If PH3 and Cl were present, their mixing ratios also increased with pressure. Species were detected at mass peaks appropriate for C2 and C3 hydrocarbons. It is not yet clear which of these were atmospheric constituents and which were instrumentally generated. These measurements imply (1) fractionation of 4He, (2) a local, altitude-dependent depletion of condensables, probably because the probe entered the descending arm of a circulation cell, (3) that icy planetesimals made significant contributions to the volatile inventory, and (4) a moderate decrease in D/H but no detectable change in (D + 3He)/H in this part of the galaxy during the past 4.6 Gyr.
Published: 2001

24. Aqueous soluble tetrazolium/formazan MTS as an indicator of NADH- and NADPH-dependent dehydrogenase activity

Author: D D, Dunigan, S B, Waters, and T C, Owen
Subjects: Dithiothreitol, Kinetics, Thiazoles, Formazans, NADPH Dehydrogenase, Methylphenazonium Methosulfate, Tetrazolium Salts, Indicators and Reagents, NADH Dehydrogenase, NAD, Oxidation-Reduction, NADP, Mercaptoethanol
Abstract: Recently a new tetrazolium was described for the use of monitoring cell viability in culture. This tetrazolium, commonly referred to as MTS [3-(4,5-dimethylthiazol-2-yl)- 5-(3-carboxymethonyphenol)-2-(4-sulfophenyl)-2H-tetrazolium, inner salt], has the unusual property that it can be reduced to a water-soluble formazan. beta-Nicotinamide adenine dinucleotide/reduced (NADH) and beta-nicotinamide adenine dinucleotide phosphate/reduced (NADPH) are examples of physiologically important reducing agents. In cell-free studies, MTS was reduce to the soluble formazan in the presence of NADH and NADPH, and reaction were compared to those with dithiothreitol (DTT) or 2-mercaptoethanol (2-ME). The efficiency of these reactions was enhanced 1000-fold by the presence of phenazine methosulfate. Selectivity in the electron transfer from NADPH was slightly greater than NADH, and NADPH or NADH was much greater than the thiols DTT or 2-ME. Generation of either NADH or NADPH in solution by malate dehydrogenase or isocitrate dehydrogenase, respectively, was monitored by the MTS reduction reaction. The rate of formazan formation was comparable to the formation of NADH or NADPH. This system represents a useful tool for evaluating reaction kinetics in solutions of NAD- or NADP-dependent dehydrogenase enzymes, and these reactions can be performed in typical biological buffers containing reducing agents without significant interference to the MTS/formazan system.
Published: 1995

25. Origin of the Major Planet Atmospheres: Clues from Trace Species

Author: S. K. Atreya, S. G. Edgington, D. Gautier, and T. C. Owen
Published: 1995

26. Organic materials in planetary and protoplanetary systems: nature or nurture?

Author: M. A. Barucci, M. Fulchignoni, Anthony P. Jones, Vito Mennella, R. Brunetto, François-Régis Orthous-Daunay, Y. J. Pendleton, C. de Bergh, Dale P. Cruikshank, William M. Grundy, Humberto Campins, C. M. Dalle Ore, Giovanni Strazzulla, John H. Debes, E. Dotto, T. C. Owen, Ilaria Pascucci, Eric Quirico, Josh Emery, and Noemi Pinilla-Alonso
Subjects: Physics, Chemical signature, Solar System, Astronomy, Astronomy and Astrophysics, Astrophysics, Planetary system, Ion bombardment, Laboratory results, Nature versus nurture, Astrobiology, Space and Planetary Science, Trans-Neptunian object, Spectral data
Abstract: Aims. The objective of this work is to summarize the discussion of a workshop aimed at investigating the properties, origins, and evolution of the materials that are responsible for the red coloration of the small objects in the outer parts of the solar system. Because of limitations or inconsistencies in the observations and, until recently, the limited availability of laboratory data, there are still many questions on the subject. Our goal is to approach two of the main questions in a systematic way: – Is coloring an original signature of materials that are presolar in origin (“nature”) or stems from post-formational chemical alteration, or weathering (“nurture”)? – What is the chemical signature of the material that causes spectra to be sloped towards the red in the visible? We examine evidence available both from the laboratory and from observations sampling different parts of the solar system and circumstellar regions (disks). Methods. We present a compilation of brief summaries gathered during the workshop and describe the evidence towards a primordial vs. evolutionary origin for the material that reddens the small objects in the outer parts of our, as well as in other, planetary systems. We proceed by first summarizing laboratory results followed by observational data collected at various distances from the Sun. Results. While laboratory experiments show clear evidence of irradiation effects, particularly from ion bombardment, the first obstacle often resides in the ability to unequivocally identify the organic material in the observations. The lack of extended spectral data of good quality and resolution is at the base of this problem. Furthermore, that both mechanisms, weathering and presolar, act on the icy materials in a spectroscopically indistinguishable way makes our goal of defining the impact of each mechanism challenging. Conclusions. Through a review of some of the workshop presentations and discussions, encompassing laboratory experiments as well as observational data, we infer that both “nature” and “nurture” are instrumental in the coloration of small objects in the outer parts
Published: 2011

27. Economics

Author: T. C. OWEN
Subjects: Sociology and Political Science, General Social Sciences
Published: 2001

28. A 3 cm sealed pyloric perforation discovered during emergency cholecystectomy

Author: Kalakata Reddy, Eoghan R T C Owen, and Eleanor Jane H Turner
Subjects: medicine.medical_specialty, medicine.diagnostic_test, business.industry, medicine.medical_treatment, Perforation (oil well), General Medicine, medicine.disease, Article, Surgery, Radiological weapon, medicine, Cholecystitis, Acute cholecystitis, Cholecystectomy, Laparoscopy, business, Laparoscopic cholecystectomy
Abstract: The diagnosis of acute cholecystitis is made on clinical, haematological, biochemical and radiological grounds, and laparoscopic cholecystectomy is commonly performed in the emergency setting. We report a case in which a patient diagnosed with acute cholecystitis was found to have a sealed pyloric perforation at laparoscopy as well as cholecystitis.
Published: 2010

29. Galileo Probe Mass Spectrometer Experiment

Author: H. B. Niemann, D. N. Harpold, S. K. Atreya, G. R. Carignan, D. M. Hunten, and T. C. Owen
Published: 1992

30. Necrotising fasciitis following inguinal hernia repair

Author: Kalakata Reddy, Eoghan R T C Owen, and Eleanor Jane H Turner
Subjects: medicine.medical_specialty, business.industry, medicine.medical_treatment, Necrotising fasciitis, General Medicine, medicine.disease, Hernia repair, Article, digestive system diseases, Surgery, stomatognathic diseases, Inguinal hernia, surgical procedures, operative, medicine, business
Abstract: We report a case of necrotising fasciitis following inguinal hernia repair. It is rare for clean operations such as hernia repair to be associated with infection, and even rarer for them to be associated with necrotising fasciitis, with only a few reports in the literature.
Published: 2009

31. The Collision of the Comet Shoemaker-Levy 9 with Jupiter: Detection and Evolution of HCN in the Stratosphere of the Planet

Author: Darrell F. Strobel, Jacques Crovisier, Daniel Gautier, G. S. Orton, Dominique Bockelée-Morvan, P. Colom, I. de Pater, H. E. Matthews, Gary R. Davis, Emmanuel Lellouch, David A. Naylor, S. K. Atreya, Matthew Joseph Griffin, A. Marten, B. Han, David B. Sanders, and T. C. Owen
Subjects: Physics, Jupiter, Planet, Comet, Astronomy, Collision, Stratosphere, Astrobiology
Published: 1995

32. Gas gangrene

Author: E R T C Owen and P J Lehner
Subjects: General Engineering, General Earth and Planetary Sciences, General Medicine, General Environmental Science
Published: 1991

33. First observations of CO and HCN on Neptune and Uranus at millimeter wavelengths and the implications for atmospheric chemistry

Author: D. Gautier, T. C. Owen, J. R. Deane, Remo P. J. Tilanus, A. Marten, S. K. Atreya, Henry E. Matthews, and D. B. Sanders
Subjects: Troposphere, Convection, Physics, Space and Planetary Science, Planet, Neptune, Atmospheric chemistry, Uranus, Astronomy, Astronomy and Astrophysics, Mini-Neptune, Stratosphere
Abstract: Observations are presented which show that CO is present in both the troposphere and stratosphere of Neptune, whereas is confined to the Neptune stratosphere with a mean mole fraction in the 0.003-30 mbar pressure level range of 1.0 x 10 exp -9. CO is present in both the stratosphere and in the troposphere with a uniformly mixed model fraction of 1.2 x 10 exp -6. Upper limits of 1.0 x 10 exp -10 and 3.0 x 10 exp -8 mole fractions are derived for HCN and CO respectively on Uranus. The origin of these species in the atmosphere of Neptune and their nondetection in that of Uranus are discussed in detail. It is concluded that the most plausible scenario involves upward convection of CO and N2 from Neptune's deep interior and a failure of chemical equilibrium at deep atmospheric levels, allowing excess CO and presumably N2 to reach the upper atmosphere. Nondetection in Uranus may be explained by the lack of a significant internal heat source in the planet and consequent suppression of vertical convection.
Published: 1993

34. Unremarkable parotid tumours that prove to be malignant

Author: E R T C Owen, A E Kark, G T Wat, and M Hob
Subjects: medicine.medical_specialty, Parotid tumours, business.industry, Parotidectomy, Parotid gland, Surgery, medicine.anatomical_structure, Histological diagnosis, medicine, Parotid Neoplasms, Recurrent tumour, business, Histological examination
Abstract: Of 539 patients with clinically unremarkable lumps treated by formal parotidectomy, subsequent histological examination indicated that 20 of these lesions were malignant. After a follow-up of 1-18 years, only one patient has suffered a recurrent tumour and none has died from disease related causes. The results indicate that formal parotidectomy is an acceptable means of treating the small number of malignant tumours presenting in this way, and strengthen the argument that attempts to obtain a histological diagnosis before treatment are contraindicated.
Published: 1991

35. Plastibell circumcision

Author: E R T C Owen and J L Kjtson
Subjects: General Medicine
Published: 1990

36. Intragastric balloons for morbid obesity

Author: E. R. T. C. Owen and A. E. Kark
Subjects: Morbid obesity, medicine.medical_specialty, business.industry, medicine, MEDLINE, Surgery, Gastric balloon, medicine.disease, business, Obesity
Published: 1990

37. Fine Needle Aspiration

Author: E R T C Owen and A E Kark
Subjects: Pathology, medicine.medical_specialty, Fine-needle aspiration, medicine.anatomical_structure, medicine.diagnostic_test, business.industry, medicine, Parotid Neoplasms, General Medicine, Differential diagnosis, business, Parotid gland
Published: 1990

38. Monodeuterated methane in the outer solar system. IV - Its detection and abundance on Neptune

Author: T. C. Owen, Jean-Pierre Maillard, C. de Bergh, and Barry L. Lutz
Subjects: Physics, Solar System, Outer planets, Extraterrestrial Environment, Astronomy, Astronomical Phenomena, Uranus, Astronomy and Astrophysics, Astrophysics, Deuterium, Atmosphere, symbols.namesake, Space and Planetary Science, Planet, Neptune, Spectroscopy, Fourier Transform Infrared, symbols, Spectral resolution, Titan (rocket family), Methane
Abstract: We have detected the 3 nu 2 band of CH3D in the spectrum of Neptune near 1.6 micrometers recorded at a spectral resolution of 4 cm-1 with the Cassegrain Fourier Transform Spectrometer at the 3.6 m Canada-France-Hawaii Telescope (CFHT) on Mauna Kea. Our analysis of this spectrum, using spectral synthesis techniques, yielded a CH3D/CH4 ratio of 6(+6)(-4) x 10(-4), which corresponds to a global D/H ratio for Neptune of 1.2(+1.2)(-0.8) x 10(-4), if CH3D is in isotopic fractionation equilibrium with HD. This value is about an order of magnitude larger than an earlier estimate by Orton et al. based on deconvolution measurements of unresolved molecular emission in the 8-10 micrometers region. Comparison of this new determination with previous studies of CH3D in the outer solar system shows that, as in the case of Uranus, the D/H on Neptune is strongly enhanced over that found on Jupiter and Saturn and is comparable to the D/H in methane on Titan and in terrestrial methane and water.
Published: 1990

39. Complications of parotid surgery

Author: E. R. T. C. Owen, N. MacGillivray, and A. E. Kark
Subjects: medicine.medical_specialty, business.industry, medicine, Surgery, business, Parotid surgery
Published: 1990

40. Observations of the UV spectrum of Saturn from 3200Å to 1400Å with the IUE

Author: John Caldwell, T. C. Owen, Garry E. Hunt, V. Moore, M. Combes, and Th. Encrenaz
Subjects: Physics, Atmospheric models, Resolution (electron density), Astronomy, Astrophysics, Atmospheric model, Spectral line, chemistry.chemical_compound, Wavelength, Geophysics, Acetylene, chemistry, Saturn, General Earth and Planetary Sciences, Absorption (electromagnetic radiation)
Abstract: Spectra of Saturn have been acquired with the IUE satellite for the 1400A to 3200A wavelength range with, at
Published: 1983

41. 16. Physical Study of Planets and Satellites (Étude Physique de Planètes et Satellites)

Author: C. H. Mayer, T. C. Owen, J. Connes, I. K. Koval, S. Miyamoto, G. H. Pettengill, S. K. Runcorn, and B. A. Smith
Published: 1976

42. A Possible Jovian Analogy to the Terrestrial Equatorial Stratospheric Wind Reversal

Author: T. C. Owen and D. O. Staley
Subjects: Atmospheric Science, Analogy, Geophysics, Jovian, Geology, Astrobiology
Published: 1963

43. Effect of vertical banded gastroplasty on the natural history of gastritis in patients with morbid obesity: a follow-up study

Author: E. R. T. C. Owen, A B Price, A C Smith, and J F Flejou
Subjects: Adult, Male, medicine.medical_specialty, Gastroenterology, Postoperative Complications, Internal medicine, Gastroscopy, medicine, Humans, Prospective Studies, Retrospective Studies, medicine.diagnostic_test, business.industry, Stomach, Intestinal metaplasia, Middle Aged, medicine.disease, Obesity, Morbid, Surgery, Endoscopy, Natural history, Gastric Dysplasia, medicine.anatomical_structure, Dysplasia, Gastritis, Female, medicine.symptom, Complication, business, Follow-Up Studies
Abstract: Vertical banded gastroplasty is an accepted surgical treatment for morbid obesity. The aim of this study was to evaluate its effect on the natural history of gastritis, as the occurrence of gastritis and dysplasia have been reported after gastric bypass, another type of bariatric surgery. Thirty-four patients who underwent vertical banded gastroplasty between 1983 and 1987 were studied, and the follow-up varied from 1 to 47 months (mean 22 months). We found no increase of gastritis and intestinal metaplasia after surgery, and we did not observe any case of gastric dysplasia. Only one patient with pre- and postoperative specimens showed a deterioration in gastric histology after surgery, and this was of a minor degree. These initial results are encouraging for surgeons interested in the treatment of morbid obesity.
Published: 1988

44. Science, surgery, and senior registrars

Author: E R T C Owen and A K Banerjee
Subjects: World Wide Web, Computer science, Correspondence, General Engineering, General Earth and Planetary Sciences, General Medicine, Data science, General Environmental Science
Published: 1989

45. Reduced products and hydrogen from x-irradiated air-saturated solutions of cystamine and cystine

Author: T C, Owen, A C, Wilbraham, J A, Roach, and D R, Ellis
Subjects: Radiation Effects, Time Factors, Taurine, Air, Cystamine, Cystine, Hydrogen Peroxide, Hydrogen-Ion Concentration, Sulfonic Acids, Oxidation-Reduction, Hydrogen
Published: 1972

46. Glutathionesulfonic acid, the predominant product of x-radiolysis of air-saturated solutions of oxidized glutathione

Author: T C, Owen and A C, Wilbraham
Subjects: Electrophoresis, Radiation Effects, Solutions, Chemistry, Time Factors, Chemical Phenomena, Taurine, Air, Water, Sulfonic Acids, Radiation Dosage, Glutathione
Published: 1972

47. Radiation-induced mixed-disulfide formation from cystamine and aliphatic disulfides in aqueous solution

Author: T C, Owen and D R, Ellis
Subjects: Oxygen, Radiation Effects, Radiochemistry, Cystamine, Ethylamines, Methods, Water, Disulfides, Acetates, Glycolates
Published: 1973

48. Role of fine needle aspiration cytology and computed tomography in the diagnosis of parotid swellings

Author: A. E. Kark, E. R. T. C. Owen, A. K. Banerjee, E. A. Hudson, and A. J. N. Prichard
Subjects: Adenoma, Adult, Male, medicine.medical_specialty, Local excision, Adolescent, Computed tomography, Pleomorphic adenoma, Fine needle aspiration cytology, Biopsy, Carcinoma, Humans, Medicine, Adenolymphoma, Aged, Aged, 80 and over, medicine.diagnostic_test, business.industry, Biopsy, Needle, Middle Aged, medicine.disease, Parotid Neoplasms, Parotid gland, Surgery, medicine.anatomical_structure, Female, Radiology, Tomography, X-Ray Computed, business
Abstract: These two investigations will provide an accurate preoperative diagnosis of the histological type and anatomical site of a parotid mass, enabling the surgeon to select those tumours, such as adenolymphoma, which require local excision only, and to avoid operative intervention for inflammatory or secondary neoplastic conditions. This approach should reduce the complications of unnecessarily extensive procedures
Published: 1989

49. Complications of parotid surgery: The need for selectivity

Author: A. E. Kark, E. R. T. C. Owen, M W Kissin, and A. K. Banerjee
Subjects: medicine.medical_specialty, business.industry, Mortality rate, Facial Paralysis, Sweating, Gustatory, Parotidectomy, medicine.disease, Facial paralysis, Parotid Neoplasms, Surgery, Parotid gland, Pleomorphic adenoma, Postoperative Complications, medicine.anatomical_structure, Superficial Parotidectomy, medicine, Humans, Parotid Gland, Complication, business, Parotid surgery
Abstract: The morbidity rate following 112 operations on the parotid gland is reported. Facial nerve palsy (temporary, 38 per cent; permanent, 9 per cent) and Frey's syndrome (11 per cent) were common following superficial parotidectomy. For pleomorphic adenoma and malignant lesions this procedure is justified. Benign conditions, which can be diagnosed preoperatively, should be treated by more limited surgery which has a lower complication rate.
Published: 1989

50. Surgery of morbid obesity

Author: A E Kark, E R T C Owen, J F Flejou, A B Price, and A C Smith
Subjects: Reoperation, medicine.medical_specialty, business.industry, medicine.medical_treatment, Jejunoileal bypass, General Engineering, General Medicine, medicine.disease, Obesity, Obesity, Morbid, Surgery, Morbid obesity, Jejunoileal Bypass, Correspondence, medicine, Humans, General Earth and Planetary Sciences, business, Digestive System Surgical Procedures, Research Article, General Environmental Science
Published: 1987

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