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Filacchione G, Raponi A, Capaccioni F, Ciarniello M, Tosi F, Capria MT, De Sanctis MC, Migliorini A, Piccioni G, Cerroni P, Barucci MA, Fornasier S, Schmitt B, Quirico E, Erard S, Bockelee-Morvan D, Leyrat C, Arnold G, Mennella V, Ammannito E, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka MI, Carlson R, Carsenty U, Colangeli L, Combes M, Combi M, Crovisier J, Drossart P, Encrenaz T, Federico C, Fink U, Fonti S, Fulchignoni M, Ip WH, Irwin P, Jaumann R, Kuehrt E, Langevin Y, Magni G, McCord T, Moroz L, Mottola S, Palomba E, Schade U, Stephan K, Taylor F, Tiphene D, Tozzi GP, Beck P, Biver N, Bonal L, Combe JP, Despan D, Flamini E, Formisano M, Frigeri A, Grassi D, Gudipati MS, Kappel D, Longobardo A, Mancarella F, Markus K, Merlin F, Orosei R, Rinaldi G, Cartacci M, Cicchetti A, Hello Y, Henry F, Jacquinod S, Reess JM, Noschese R, Politi R, Peter G. Seasonal exposure of carbon dioxide ice on the nucleus of comet 67P/Churyumov-Gerasimenko. Science 2016; 354:1563-1566. [DOI: 10.1126/science.aag3161] [Citation(s) in RCA: 49] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/08/2016] [Accepted: 10/28/2016] [Indexed: 11/02/2022]
Affiliation(s)
- G. Filacchione
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Raponi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Capaccioni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. Ciarniello
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Tosi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. T. Capria
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. C. De Sanctis
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Migliorini
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - G. Piccioni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - P. Cerroni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. A. Barucci
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - S. Fornasier
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - B. Schmitt
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - E. Quirico
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - S. Erard
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - D. Bockelee-Morvan
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - C. Leyrat
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - G. Arnold
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - V. Mennella
- INAF Osservatorio di Capodimonte, Naples, Italy
| | - E. Ammannito
- Department of Earth, Planetary, and Space Sciences, University of California–Los Angeles, 603 Charles Young Drive, Los Angeles, CA 90095-1567, USA
| | - G. Bellucci
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - J. Benkhoff
- ESA (European Space Agency), European Space Research and Technology Centre, Noordwjik, Netherlands
| | - J. P. Bibring
- Institut d’Astrophysique Spatial, CNRS, Orsay, France
| | - A. Blanco
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - M. I. Blecka
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | - R. Carlson
- NASA JPL (Jet Propulsion Laboratory), California Institute of Technology, Pasadena, CA 91109, USA
| | - U. Carsenty
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - L. Colangeli
- ESA (European Space Agency), European Space Research and Technology Centre, Noordwjik, Netherlands
| | - M. Combes
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - M. Combi
- Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA
| | - J. Crovisier
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - P. Drossart
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - T. Encrenaz
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | | | - U. Fink
- Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - S. Fonti
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - M. Fulchignoni
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - W.-H. Ip
- National Central University, Taipei, Taiwan
| | - P. Irwin
- Departement of Physics, Oxford University, Oxford, UK
| | - R. Jaumann
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - E. Kuehrt
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - Y. Langevin
- Institut d’Astrophysique Spatial, CNRS, Orsay, France
| | - G. Magni
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - T. McCord
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - L. Moroz
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - S. Mottola
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - E. Palomba
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - U. Schade
- Helmholtz-Zentrum Berlin für Materialien und Energie, Berlin, Germany
| | - K. Stephan
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - F. Taylor
- Departement of Physics, Oxford University, Oxford, UK
| | - D. Tiphene
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - G. P. Tozzi
- INAF Osservatorio Astrofisico di Arcetri, Firenze, Italy
| | - P. Beck
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | - N. Biver
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - L. Bonal
- Université Grenoble Alpes, CNRS, Institut de Planetologie et d’Astrophysique de Grenoble, Grenoble, France
| | | | - D. Despan
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | | | - M. Formisano
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Frigeri
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - D. Grassi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. S. Gudipati
- NASA JPL (Jet Propulsion Laboratory), California Institute of Technology, Pasadena, CA 91109, USA
| | - D. Kappel
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - A. Longobardo
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - F. Mancarella
- Dipartimento di Matematica e Fisica “Ennio De Giorgi,” Università del Salento, Lecce, Italy
| | - K. Markus
- Institute for Planetary Research, DLR (Deutschen Zentrums für Luft- und Raumfahrt), Berlin, Germany
| | - F. Merlin
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - R. Orosei
- INAF Istituto di Radioastronomia, Bologna, Italy
| | - G. Rinaldi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - M. Cartacci
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - A. Cicchetti
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - Y. Hello
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - F. Henry
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - S. Jacquinod
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - J. M. Reess
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Paris Sciences and Letters Research University, CNRS (Centre National de la Recherche Scientifique), Sorbonne Universités, UPMC (Université Pierre et Marie Curie) Université Paris 06, Université Paris Diderot, Sorbonne Paris Cité, France
| | - R. Noschese
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - R. Politi
- INAF-IAPS (Istituto Nazionale di AstroFisica–Istituto di Astrofisica e Planetologia Spaziali), Rome, Italy
| | - G. Peter
- Institute of Optical Sensor Systems, DLR, Berlin, Germany
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Capaccioni F, Coradini A, Filacchione G, Erard S, Arnold G, Drossart P, De Sanctis MC, Bockelee-Morvan D, Capria MT, Tosi F, Leyrat C, Schmitt B, Quirico E, Cerroni P, Mennella V, Raponi A, Ciarniello M, McCord T, Moroz L, Palomba E, Ammannito E, Barucci MA, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka M, Carlson R, Carsenty U, Colangeli L, Combes M, Combi M, Crovisier J, Encrenaz T, Federico C, Fink U, Fonti S, Ip WH, Irwin P, Jaumann R, Kuehrt E, Langevin Y, Magni G, Mottola S, Orofino V, Palumbo P, Piccioni G, Schade U, Taylor F, Tiphene D, Tozzi GP, Beck P, Biver N, Bonal L, Combe JP, Despan D, Flamini E, Fornasier S, Frigeri A, Grassi D, Gudipati M, Longobardo A, Markus K, Merlin F, Orosei R, Rinaldi G, Stephan K, Cartacci M, Cicchetti A, Giuppi S, Hello Y, Henry F, Jacquinod S, Noschese R, Peter G, Politi R, Reess JM, Semery A. Cometary science. The organic-rich surface of comet 67P/Churyumov-Gerasimenko as seen by VIRTIS/Rosetta. Science 2015; 347:aaa0628. [PMID: 25613895 DOI: 10.1126/science.aaa0628] [Citation(s) in RCA: 266] [Impact Index Per Article: 29.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 ± 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% kÅ(-1)), and the broad absorption feature in the 2.9-to-3.6-micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.
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Affiliation(s)
- F Capaccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy.
| | - A Coradini
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - G Filacchione
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Erard
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G Arnold
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - P Drossart
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M C De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - D Bockelee-Morvan
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M T Capria
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - C Leyrat
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - B Schmitt
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - E Quirico
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - P Cerroni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - V Mennella
- Osservatorio di Capodimonte, INAF, Napoli, Italy
| | - A Raponi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - M Ciarniello
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - T McCord
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - L Moroz
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - E Palomba
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - E Ammannito
- University of California, Los Angeles, Los Angeles, CA 90095, USA
| | - M A Barucci
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G Bellucci
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - J Benkhoff
- European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands
| | - J P Bibring
- Institut d'Astrophysique Spatial, CNRS, Orsay, France
| | - A Blanco
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - M Blecka
- Space Research Centre, Polish Academy of Sciences, Warsaw, Poland
| | - R Carlson
- NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA
| | - U Carsenty
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - L Colangeli
- European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands
| | - M Combes
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - M Combi
- Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA
| | - J Crovisier
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - T Encrenaz
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | | | - U Fink
- Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - S Fonti
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - W H Ip
- National Central University, Taipei, Taiwan
| | - P Irwin
- Departement of Physics, Oxford University, Oxford, UK
| | - R Jaumann
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany. Free University of Berlin, Institute of Geosciences, Malteserstraße 74-100, Building Haus A, 12249 Berlin, Germany
| | - E Kuehrt
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - Y Langevin
- Institut d'Astrophysique Spatial, CNRS, Orsay, France
| | - G Magni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Mottola
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - V Orofino
- Dipartimento di Matematica e Fisica "Ennio De Giorgi," Università del Salento, Italy
| | - P Palumbo
- Università "Parthenope," Napoli, Italy
| | - G Piccioni
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - U Schade
- Helmholtz-Zentrum Berlin für Materialien und Energie, Berlin, Germany
| | - F Taylor
- Departement of Physics, Oxford University, Oxford, UK
| | - D Tiphene
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - G P Tozzi
- Osservatorio Astrofisico di Arcetri, INAF, Firenze, Italy
| | - P Beck
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - N Biver
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - L Bonal
- Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique de Grenoble, Grenoble, France
| | - J-Ph Combe
- Bear Fight Institute, Winthrop, WA 98862, USA
| | - D Despan
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - E Flamini
- Agenzia Spaziale Italiana, Rome, Italy
| | - S Fornasier
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - A Frigeri
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - D Grassi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - M Gudipati
- NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, USA
| | - A Longobardo
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - K Markus
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - F Merlin
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - R Orosei
- Istituto di Radioastronomia, INAF, Bologna, Italy
| | - G Rinaldi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - K Stephan
- Institute for Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Berlin, Germany
| | - M Cartacci
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - A Cicchetti
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - S Giuppi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - Y Hello
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - F Henry
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - S Jacquinod
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - R Noschese
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - G Peter
- Institut für Optische Sensorsysteme, DLR, Berlin, Germany
| | - R Politi
- Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy
| | - J M Reess
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
| | - A Semery
- Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Université Pierre et Marie Curie[acute accent over last letter in "Université"]/Université Paris-Diderot, Meudon, France
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3
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Coradini A, Capaccioni F, Erard S, Arnold G, De Sanctis MC, Filacchione G, Tosi F, Barucci MA, Capria MT, Ammannito E, Grassi D, Piccioni G, Giuppi S, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka M, Bockelee-Morvan D, Carraro F, Carlson R, Carsenty U, Cerroni P, Colangeli L, Combes M, Combi M, Crovisier J, Drossart P, Encrenaz ET, Federico C, Fink U, Fonti S, Giacomini L, Ip WH, Jaumann R, Kuehrt E, Langevin Y, Magni G, McCord T, Mennella V, Mottola S, Neukum G, Orofino V, Palumbo P, Schade U, Schmitt B, Taylor F, Tiphene D, Tozzi G. The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS. Science 2011; 334:492-4. [DOI: 10.1126/science.1204062] [Citation(s) in RCA: 98] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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4
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Luz D, Berry DL, Piccioni G, Drossart P, Politi R, Wilson CF, Erard S, Nuccilli F. Venus’s Southern Polar Vortex Reveals Precessing Circulation. Science 2011; 332:577-80. [DOI: 10.1126/science.1201629] [Citation(s) in RCA: 47] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- D. Luz
- Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, 1349-018 Lisboa, Portugal
| | - D. L. Berry
- Departamento de Física, Universidade de Évora, 7002-554 Évora, Portugal
| | - G. Piccioni
- Istituto Nazionale di Astrofisica, Istituto Nazionale di Astrofisica– Istituto di Astrofisica Spaziale e Fisica Cosmica (INAF-IASF) Rome, 00133 Rome, Italy
| | - P. Drossart
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Université Pierre et Marie Curie, Université Paris-Diderot, F-92195 Meudon Cedex, France
| | - R. Politi
- Istituto Nazionale di Astrofisica, Istituto Nazionale di Astrofisica– Istituto di Astrofisica Spaziale e Fisica Cosmica (INAF-IASF) Rome, 00133 Rome, Italy
| | - C. F. Wilson
- Department of Physics, University of Oxford, Oxford OX1 3PU, UK
| | - S. Erard
- Laboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, CNRS, Université Pierre et Marie Curie, Université Paris-Diderot, F-92195 Meudon Cedex, France
| | - F. Nuccilli
- INAF–Istituto di Fisica dello Spazio Interplanetario (IFSI) Rome, 00133 Rome, Italy
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5
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Grassi D, Migliorini A, Montabone L, Lebonnois S, Cardesìn-Moinelo A, Piccioni G, Drossart P, Zasova LV. Thermal structure of Venusian nighttime mesosphere as observed by VIRTIS-Venus Express. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003553] [Citation(s) in RCA: 36] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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6
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García Muñoz A, Mills FP, Slanger TG, Piccioni G, Drossart P. Visible and near-infrared nightglow of molecular oxygen in the atmosphere of Venus. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003447] [Citation(s) in RCA: 52] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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7
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Gérard JC, Cox C, Soret L, Saglam A, Piccioni G, Bertaux JL, Drossart P. Concurrent observations of the ultraviolet nitric oxide and infrared O2nightglow emissions with Venus Express. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003371] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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8
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Ignatiev NI, Titov DV, Piccioni G, Drossart P, Markiewicz WJ, Cottini V, Roatsch T, Almeida M, Manoel N. Altimetry of the Venus cloud tops from the Venus Express observations. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003320] [Citation(s) in RCA: 111] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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9
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Piccioni G, Zasova L, Migliorini A, Drossart P, Shakun A, García Muñoz A, Mills FP, Cardesin‐Moinelo A. Near‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003133] [Citation(s) in RCA: 69] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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10
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Satoh T, Imamura T, Hashimoto GL, Iwagami N, Mitsuyama K, Sorahana S, Drossart P, Piccioni G. Cloud structure in Venus middle‐to‐lower atmosphere as inferred from VEX/VIRTIS 1.74μm data. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003184] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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11
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Garcia RF, Drossart P, Piccioni G, López-Valverde M, Occhipinti G. Gravity waves in the upper atmosphere of Venus revealed by CO2nonlocal thermodynamic equilibrium emissions. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003073] [Citation(s) in RCA: 27] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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12
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Gilli G, López-Valverde MA, Drossart P, Piccioni G, Erard S, Cardesín Moinelo A. Limb observations of CO2and CO non-LTE emissions in the Venus atmosphere by VIRTIS/Venus Express. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003112] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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García Muñoz A, Mills FP, Piccioni G, Drossart P. The near-infrared nitric oxide nightglow in the upper atmosphere of Venus. Proc Natl Acad Sci U S A 2009; 106:985-8. [PMID: 19164595 PMCID: PMC2633570 DOI: 10.1073/pnas.0808091106] [Citation(s) in RCA: 42] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/15/2008] [Indexed: 11/18/2022] Open
Abstract
The v' = 0 progressions of the C --> X and A --> X band systems of nitric oxide dominate the middle-UV spectrum of the night-time upper atmospheres of the Earth, Mars, and Venus. The C(0) --> A(0)+h nu radiative transition at 1.224 mum, the only channel effectively populating the A(0) level, must therefore occur also. There have been, however, no reported detections of the C(0) --> A(0) band in the atmospheres of these or any other planets. We analyzed all available near-infrared limb observations of the dark-side atmosphere of Venus by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument on the Venus Express spacecraft and found 2 unambiguous detections of this band at equatorial latitudes that seem to be associated with episodic events of highly enhanced nightglow emission. The discovery of the C(0) --> A(0) band means observations in the 1.2-1.3 microm region, which also contains the a(0) --> X(0) emission band of molecular oxygen, can provide a wealth of information on the high-altitude chemistry and dynamics of the Venusian atmosphere.
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Affiliation(s)
- A García Muñoz
- Research School of Physics and Engineering, Australian National University, Canberra, ACT 0200, Australia.
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14
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Erard S, Drossart P, Piccioni G. Multivariate analysis of Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) Venus Express nightside and limb observations. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003116] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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15
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Peralta J, Hueso R, Sánchez-Lavega A, Piccioni G, Lanciano O, Drossart P. Characterization of mesoscale gravity waves in the upper and lower clouds of Venus from VEX-VIRTIS images. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003185] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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Mueller N, Helbert J, Hashimoto GL, Tsang CCC, Erard S, Piccioni G, Drossart P. Venus surface thermal emission at 1μm in VIRTIS imaging observations: Evidence for variation of crust and mantle differentiation conditions. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003118] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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Wilson CF, Guerlet S, Irwin PGJ, Tsang CCC, Taylor FW, Carlson RW, Drossart P, Piccioni G. Evidence for anomalous cloud particles at the poles of Venus. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003108] [Citation(s) in RCA: 33] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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18
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Piccialli A, Titov DV, Grassi D, Khatuntsev I, Drossart P, Piccioni G, Migliorini A. Cyclostrophic winds from the Visible and Infrared Thermal Imaging Spectrometer temperature sounding: A preliminary analysis. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003127] [Citation(s) in RCA: 27] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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19
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Grassi D, Drossart P, Piccioni G, Ignatiev NI, Zasova LV, Adriani A, Moriconi ML, Irwin PGJ, Negrão A, Migliorini A. Retrieval of air temperature profiles in the Venusian mesosphere from VIRTIS-M data: Description and validation of algorithms. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003075] [Citation(s) in RCA: 26] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Marcq E, Bézard B, Drossart P, Piccioni G, Reess JM, Henry F. A latitudinal survey of CO, OCS, H2O, and SO2in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS-H. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003074] [Citation(s) in RCA: 64] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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21
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Hueso R, Sánchez-Lavega A, Piccioni G, Drossart P, Gérard JC, Khatuntsev I, Zasova L, Migliorini A. Morphology and dynamics of Venus oxygen airglow from Venus Express/Visible and Infrared Thermal Imaging Spectrometer observations. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003081] [Citation(s) in RCA: 44] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Irwin PGJ, de Kok R, Negrão A, Tsang CCC, Wilson CF, Drossart P, Piccioni G, Grassi D, Taylor FW. Spatial variability of carbon monoxide in Venus' mesosphere from Venus Express/Visible and Infrared Thermal Imaging Spectrometer measurements. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003093] [Citation(s) in RCA: 43] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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23
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Montmessin F, Gondet B, Bibring JP, Langevin Y, Drossart P, Forget F, Fouchet T. Hyperspectral imaging of convective CO2ice clouds in the equatorial mesosphere of Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002944] [Citation(s) in RCA: 65] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Cruikshank DP, Dalton JB, Dalle Ore CM, Bauer J, Stephan K, Filacchione G, Hendrix AR, Hansen CJ, Coradini A, Cerroni P, Tosi F, Capaccioni F, Jaumann R, Buratti BJ, Clark RN, Brown RH, Nelson RM, McCord TB, Baines KH, Nicholson PD, Sotin C, Meyer AW, Bellucci G, Combes M, Bibring JP, Langevin Y, Sicardy B, Matson DL, Formisano V, Drossart P, Mennella V. Surface composition of Hyperion. Nature 2007; 448:54-6. [PMID: 17611536 DOI: 10.1038/nature05948] [Citation(s) in RCA: 45] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/09/2007] [Accepted: 05/16/2007] [Indexed: 11/09/2022]
Abstract
Hyperion, Saturn's eighth largest icy satellite, is a body of irregular shape in a state of chaotic rotation. The surface is segregated into two distinct units. A spatially dominant high-albedo unit having the strong signature of H2O ice contrasts with a unit that is about a factor of four lower in albedo and is found mostly in the bottoms of cup-like craters. Here we report observations of Hyperion's surface in the ultraviolet and near-infrared spectral regions with two optical remote sensing instruments on the Cassini spacecraft at closest approach during a fly-by on 25-26 September 2005. The close fly-by afforded us the opportunity to obtain separate reflectance spectra of the high- and low-albedo surface components. The low-albedo material has spectral similarities and compositional signatures that link it with the surface of Phoebe and a hemisphere-wide superficial coating on Iapetus.
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Affiliation(s)
- D P Cruikshank
- NASA Ames Research Center, MS 245-6, NASA Ames Research Center, MS 211-3, Moffett Field, California 94035, USA.
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25
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Negrão A, Hirtzig M, Coustenis A, Gendron E, Drossart P, Rannou P, Combes M, Boudon V. The 2-μm spectroscopy of Huygens probe landing site on Titan with Very Large Telescope/Nasmyth Adaptive Optics System Near-Infrared Imager and Spectrograph. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2005je002651] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Hirtzig M, Coustenis A, Gendron E, Drossart P, Hartung M, Negrão A, Rannou P, Combes M. Titan: Atmospheric and surface features as observed with Nasmyth Adaptive Optics System Near-Infrared Imager and Spectrograph at the time of the Huygens mission. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2005je002650] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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27
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Griffith CA, Penteado P, Rannou P, Brown R, Boudon V, Baines KH, Clark R, Drossart P, Buratti B, Nicholson P, McKay CP, Coustenis A, Negrao A, Jaumann R. Evidence for a Polar Ethane Cloud on Titan. Science 2006; 313:1620-2. [PMID: 16973876 DOI: 10.1126/science.1128245] [Citation(s) in RCA: 147] [Impact Index Per Article: 8.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal the presence of a vast tropospheric cloud on Titan at latitudes 51 degrees to 68 degrees north and all longitudes observed (10 degrees to 190 degrees west). The derived characteristics indicate that this cloud is composed of ethane and forms as a result of stratospheric subsidence and the particularly cool conditions near the moon's north pole. Preferential condensation of ethane, perhaps as ice, at Titan's poles during the winters may partially explain the lack of liquid ethane oceans on Titan's surface at middle and lower latitudes.
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Affiliation(s)
- C A Griffith
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85721 USA
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28
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Brown RH, Clark RN, Buratti BJ, Cruikshank DP, Barnes JW, Mastrapa RME, Bauer J, Newman S, Momary T, Baines KH, Bellucci G, Capaccioni F, Cerroni P, Combes M, Coradini A, Drossart P, Formisano V, Jaumann R, Langevin Y, Matson DL, McCord TB, Nelson RM, Nicholson PD, Sicardy B, Sotin C. Composition and Physical Properties of Enceladus' Surface. Science 2006; 311:1425-8. [PMID: 16527972 DOI: 10.1126/science.1121031] [Citation(s) in RCA: 170] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Observations of Saturn's satellite Enceladus using Cassini's Visual and Infrared Mapping Spectrometer instrument were obtained during three flybys of Enceladus in 2005. Enceladus' surface is composed mostly of nearly pure water ice except near its south pole, where there are light organics, CO2, and amorphous and crystalline water ice, particularly in the region dubbed the "tiger stripes." An upper limit of 5 precipitable nanometers is derived for CO in the atmospheric column above Enceladus, and 2% for NH3 in global surface deposits. Upper limits of 140 kelvin (for a filled pixel) are derived for the temperatures in the tiger stripes.
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Affiliation(s)
- Robert H Brown
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
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29
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Poulet F, Bibring JP, Mustard JF, Gendrin A, Mangold N, Langevin Y, Arvidson RE, Gondet B, Gomez C, Berthé M, Erard S, Forni O, Manaud N, Poulleau G, Soufflot A, Combes M, Drossart P, Encrenaz T, Fouchet T, Melchiorri R, Bellucci G, Altieri F, Formisano V, Fonti S, Capaccioni F, Cerroni P, Coradini A, Korablev O, Kottsov V, Ignatiev N, Titov D, Zasova L, Pinet P, Schmitt B, Sotin C, Hauber E, Hoffmann H, Jaumann R, Keller U, Forget F. Phyllosilicates on Mars and implications for early martian climate. Nature 2005; 438:623-7. [PMID: 16319882 DOI: 10.1038/nature04274] [Citation(s) in RCA: 175] [Impact Index Per Article: 9.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2005] [Accepted: 09/27/2005] [Indexed: 11/09/2022]
Abstract
The recent identification of large deposits of sulphates by remote sensing and in situ observations has been considered evidence of the past presence of liquid water on Mars. Here we report the unambiguous detection of diverse phyllosilicates, a family of aqueous alteration products, on the basis of observations by the OMEGA imaging spectrometer on board the Mars Express spacecraft. These minerals are mainly associated with Noachian outcrops, which is consistent with an early active hydrological system, sustaining the long-term contact of igneous minerals with liquid water. We infer that the two main families of hydrated alteration products detected-phyllosilicates and sulphates--result from different formation processes. These occurred during two distinct climatic episodes: an early Noachian Mars, resulting in the formation of hydrated silicates, followed by a more acidic environment, in which sulphates formed.
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Affiliation(s)
- F Poulet
- Institut d'Astrophysique Spatiale, Université Paris-Sud and CNRS (UMR 8617) F-91405 Orsay, France.
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30
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Griffith CA, Penteado P, Baines K, Drossart P, Barnes J, Bellucci G, Bibring J, Brown R, Buratti B, Capaccioni F, Cerroni P, Clark R, Combes M, Coradini A, Cruikshank D, Formisano V, Jaumann R, Langevin Y, Matson D, McCord T, Mennella V, Nelson R, Nicholson P, Sicardy B, Sotin C, Soderblom LA, Kursinski R. The evolution of Titan's mid-latitude clouds. Science 2005; 310:474-7. [PMID: 16239472 DOI: 10.1126/science.1117702] [Citation(s) in RCA: 123] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal that the horizontal structure, height, and optical depth of Titan's clouds are highly dynamic. Vigorous cloud centers are seen to rise from the middle to the upper troposphere within 30 minutes and dissipate within the next hour. Their development indicates that Titan's clouds evolve convectively; dissipate through rain; and, over the next several hours, waft downwind to achieve their great longitude extents. These and other characteristics suggest that temperate clouds originate from circulation-induced convergence, in addition to a forcing at the surface associated with Saturn's tides, geology, and/or surface composition.
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Affiliation(s)
- C A Griffith
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
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Sotin C, Jaumann R, Buratti BJ, Brown RH, Clark RN, Soderblom LA, Baines KH, Bellucci G, Bibring JP, Capaccioni F, Cerroni P, Combes M, Coradini A, Cruikshank DP, Drossart P, Formisano V, Langevin Y, Matson DL, McCord TB, Nelson RM, Nicholson PD, Sicardy B, LeMouelic S, Rodriguez S, Stephan K, Scholz CK. Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan. Nature 2005; 435:786-9. [PMID: 15944697 DOI: 10.1038/nature03596] [Citation(s) in RCA: 174] [Impact Index Per Article: 9.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/27/2004] [Accepted: 03/24/2005] [Indexed: 11/09/2022]
Abstract
Titan is the only satellite in our Solar System with a dense atmosphere. The surface pressure is 1.5 bar (ref. 1) and, similar to the Earth, N2 is the main component of the atmosphere. Methane is the second most important component, but it is photodissociated on a timescale of 10(7) years (ref. 3). This short timescale has led to the suggestion that Titan may possess a surface or subsurface reservoir of hydrocarbons to replenish the atmosphere. Here we report near-infrared images of Titan obtained on 26 October 2004 by the Cassini spacecraft. The images show that a widespread methane ocean does not exist; subtle albedo variations instead suggest topographical variations, as would be expected for a more solid (perhaps icy) surface. We also find a circular structure approximately 30 km in diameter that does not resemble any features seen on other icy satellites. We propose that the structure is a dome formed by upwelling icy plumes that release methane into Titan's atmosphere.
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Affiliation(s)
- C Sotin
- Laboratoire de Planétologie et Géodynamique, UMR CNRS 6112, Université de Nantes, Nantes, 44100, France.
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32
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Bibring JP, Langevin Y, Gendrin A, Gondet B, Poulet F, Berthé M, Soufflot A, Arvidson R, Mangold N, Mustard J, Drossart P. Mars Surface Diversity as Revealed by the OMEGA/Mars Express Observations. Science 2005; 307:1576-81. [PMID: 15718430 DOI: 10.1126/science.1108806] [Citation(s) in RCA: 198] [Impact Index Per Article: 10.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Observatoire pour la Minéralogie, l'Eau, les Glaces, et l'Activité (OMEGA) investigation, on board the European Space Agency Mars Express mission, is mapping the surface composition of Mars at a 0.3- to 5-kilometer resolution by means of visible-near-infrared hyperspectral reflectance imagery. The data acquired during the first 9 months of the mission already reveal a diverse and complex surface mineralogy, offering key insights into the evolution of Mars. OMEGA has identified and mapped mafic iron-bearing silicates of both the northern and southern crust, localized concentrations of hydrated phyllosilicates and sulfates but no carbonates, and ices and frosts with a water-ice composition of the north polar perennial cap, as for the south cap, covered by a thin carbon dioxide-ice veneer.
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Affiliation(s)
- Jean-Pierre Bibring
- Institut d'Astrophysique Spatiale (IAS), Bâtiment 121, 91405 Orsay Campus, France.
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33
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Cottaz C, Kleiner I, Tarrago G, Brown LR, Margolis JS, Poynter RL, Pickett HM, Fouchet T, Drossart P, Lellouch E. Line Positions and Intensities in the 2nu(2)/nu(4) Vibrational System of (14)NH(3) near 5-7 µm. J Mol Spectrosc 2000; 203:285-309. [PMID: 10986141 DOI: 10.1006/jmsp.2000.8182] [Citation(s) in RCA: 33] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Line positions and intensities belonging to the vibrational system 2nu(2)/nu(4) of ammonia (14)NH(3) are measured and analyzed between 1200 and 2200 cm(-1) in order to improve the molecular database. For this, laboratory spectra are obtained at 0.006 and 0.011 cm(-1) unapodized resolution and with 4% precisions for the intensities using Fourier transform spectrometers located at the Kitt Peak National Observatory and the Jet Propulsion Laboratory. The observed data contain transitions of the nu(4) fundamental band near 1626.276(1) and 1627.375(2) cm(-1) (for s and a inversion upper states, respectively) and the 2nu(2) overtone band near 1597.470(3) and 1882.179(5) cm(-1) (for s and a inversion states, respectively). A total of 2345 lines with J' </= 15 is assigned from which 2114 line positions with J' </= 15 are fitted using an effective rotation-inversion-rotation Hamiltonian to achieve an rms of 0.003 cm(-1) with 57 molecular parameters. Over 1200 intensity measurements are modeled to +/-4.7% using 16 terms of the dipole moment expansion. A dyad model is used in order to model all the interactions expected within the 2nu(2)/nu(4) system. The bandstrengths of 2nu(2) (s <-- a), 2nu(2) (a <-- s), and nu(4) (s <-- s and a <-- a) are estimated to be 6.68(24), 0.201(5), and 116(3) cm(-2) atm(-1), respectively, at 296 K. The prediction generated by this study is available for planetary studies. Copyright 2000 Academic Press.
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Affiliation(s)
- C Cottaz
- Laboratoire de Photophysique Moléculaire, Université Paris Sud, Unité propre de C.N.R.S., Bâtiment 210, Orsay Cédex, 91405, France
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34
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Roos-Serote M, Vasavada AR, Kamp L, Drossart P, Irwin P, Nixon C, Carlson RW. Proximate humid and dry regions in Jupiter's atmosphere indicate complex local meteorology. Nature 2000; 405:158-60. [PMID: 10821265 DOI: 10.1038/35012023] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
Models of Jupiter's formation and structure predict that its atmosphere is enriched in oxygen, relative to the Sun, and that consequently water clouds should be present globally near the 5-bar pressure level. Past attempts to confirm these predictions have led to contradictory results; in particular, the Galileo probe revealed a very dry atmosphere at the entry site, with no significant clouds at depths exceeding the 2-bar level. Although the entry site was known to be relatively cloud-free, the contrast between the observed local dryness and the expected global wetness was surprising. Here we analyse near-infrared (around 5 microm) observations of Jupiter, a spectral region that can reveal the water vapour abundance and vertical cloud structure in the troposphere. We find that humid and extremely dry regions exist in close proximity, and that some humid regions are spatially correlated with bright convective clouds extending from the deep water clouds to the visible atmosphere.
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Affiliation(s)
- M Roos-Serote
- Observatório Astronómico de Lisboa, Tapada da Ajuda, Lisbon, Portugal.
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35
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Atreya SK, Wong MH, Owen TC, Mahaffy PR, Niemann HB, de Pater I, Drossart P, Encrenaz TH. A comparison of the atmospheres of Jupiter and Saturn: deep atmospheric composition, cloud structure, vertical mixing, and origin. Planet Space Sci 1999; 47:1243-1262. [PMID: 11543193 DOI: 10.1016/s0032-0633(99)00047-1] [Citation(s) in RCA: 19] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
We present our current understanding of the composition, vertical mixing, cloud structure and the origin of the atmospheres of Jupiter and Saturn. Available observations point to a much more vigorous vertical mixing in Saturn's middle-upper atmosphere than in Jupiter's. The nearly cloud-free nature of the Galileo probe entry site, a 5-micron hotspot, is consistent with the depletion of condensable volatiles to great depths, which is attributed to local meteorology. Somewhat similar depletion of water may be present in the 5-micron bright regions of Saturn also. The supersolar abundances of heavy elements, particularly C and S in Jupiter's atmosphere and C in Saturn's, as well as the progressive increase of C from Jupiter to Saturn and beyond, tend to support the icy planetesimal model of the formation of the giant planets and their atmospheres. However, much work remains to be done, especially in the area of laboratory studies, including identification of possible new microwave absorbers, and modelling, in order to resolve the controversy surrounding the large discrepancy between Jupiter's global ammonia abundance, hence the nitrogen elemental ratio, derived from the earth-based microwave observations and that inferred from the analysis of the Galileo probe-orbiter radio attenuation data for the hotspot. We look forward to the observations from Cassini-Huygens spacecraft which are expected to result not only in a rich harvest of information for Saturn, but a better understanding of the formation of the giant planets and their atmospheres when these data are combined with those that exist for Jupiter.
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Affiliation(s)
- S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, The University of Michigan, Ann Arbor 48109-2143, USA.
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36
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Roos-Serote M, Drossart P, Encrenaz T, Lellouch E, Carlson RW, Baines KH, Kamp L, Mehlman R, Orton GS, Calcutt S, Irwin P, Taylor F, Weir A. Analysis of Jupiter north equatorial belt hot spots in the 4-5 μm range from Galileo/near-infrared mapping spectrometer observations: Measurements of cloud opacity, water, and ammonia. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je01049] [Citation(s) in RCA: 49] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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37
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Irwin PGJ, Weir AL, Smith SE, Taylor FW, Lambert AL, Calcutt SB, Cameron-Smith PJ, Carlson RW, Baines K, Orton GS, Drossart P, Encrenaz T, Roos-Serote M. Cloud structure and atmospheric composition of Jupiter retrieved from Galileo near-infrared mapping spectrometer real-time spectra. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je00948] [Citation(s) in RCA: 62] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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38
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Waite JH, Gladstone GR, Lewis WS, Drossart P, Cravens TE, Maurellis AN, Mauk BH, Miller S. Equatorial X-ray Emissions: Implications for Jupiter's High Exospheric Temperatures. Science 1997; 276:104-8. [PMID: 9082978 DOI: 10.1126/science.276.5309.104] [Citation(s) in RCA: 79] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
Observations with the High Resolution Imager on the Rontgensatellit reveal x-ray emissions from Jupiter's equatorial latitudes. The observed emissions probably result from the precipitation of energetic (>300 kiloelectron volts per atomic mass unit) sulfur and oxygen ions out of Jupiter's inner radiation belt. Model calculations of the energy deposition by such heavy ion precipitation and of the resulting atmospheric heating rates indicate that this energy source can contribute to the high exospheric temperatures(>800 kelvin at 0.01 microbar) measured by the Galileo probe's Atmospheric Structure Instrument. Low-latitude energetic particle precipitation must therefore be considered, in addition to other proposed mechanisms such as gravity waves and soft electron precipitation, as an important source of heat for Jupiter's thermosphere.
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Affiliation(s)
- JH Waite
- J. H. Waite Jr., G. R. Gladstone, W. S. Lewis, Department of Space Science, Southwest Research Institute, Post Office Box 28510, San Antonio, TX 78228-0510, USA. P. Drossart, DESPA, Observatoire de Paris, F-92195 Meudon Cedex, France. T. E. Cravens and A. N. Maurellis, Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045-2151, USA. B. H. Mauk, Applied Physics Laboratory, The Johns Hopkins University, Laurel, MD 20723-6099, USA. S. Miller, Department of History, Philosophy, and Communication in Science, University College London, London WC1E 6BT, UK
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Carlson R, Smythe W, Baines K, Barbinis E, Becker K, Burns R, Calcutt S, Calvin W, Clark R, Danielson G, Davies A, Drossart P, Encrenaz T, Fanale F, Granahan J, Hansen G, Herrera P, Hibbitts C, Hui J, Irwin P, Johnson T, Kamp L, Kieffer H, Leader F, Weissman P. Near-infrared spectroscopy and spectral mapping of Jupiter and the Galilean satellites: results from Galileo's initial orbit. Science 1996; 274:385-8. [PMID: 8832878 DOI: 10.1126/science.274.5286.385] [Citation(s) in RCA: 131] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/02/2023]
Abstract
The Near Infrared Mapping Spectrometer performed spectral studies of Jupiter and the Galilean satellites during the June 1996 perijove pass of the Galileo spacecraft. Spectra for a 5-micrometer hot spot on Jupiter are consistent with the absence of a significant water cloud above 8 bars and with a depletion of water compared to that predicted for solar composition, corroborating results from the Galileo probe. Great Red Spot (GRS) spectral images show that parts of this feature extend upward to 240 millibars, although considerable altitude-dependent structure is found within it. A ring of dense clouds surrounds the GRS and is lower than it by 3 to 7 kilometers. Spectra of Callisto and Ganymede reveal a feature at 4. 25 micrometers, attributed to the presence of hydrated minerals or possibly carbon dioxide on their surfaces. Spectra of Europa's high latitudes imply that fine-grained water frost overlies larger grains. Several active volcanic regions were found on Io, with temperatures of 420 to 620 kelvin and projected areas of 5 to 70 square kilometers.
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Affiliation(s)
- R Carlson
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena 91109, USA
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40
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Orton G, Ortiz JL, Baines K, Bjoraker G, Carsenty U, Colas F, Dayal A, Deming D, Drossart P, Frappa E, Friedson J, Goguen J, Golisch W, Griep D, Hernandez C, Hoffmann W, Jennings D, Kaminski C, Kuhn J, Laques P, Limaye S, Lin H, Lecacheux J, Martin T, McCabe G, Momary T, Parker D, Puetter R, Ressler M, Reyes G, Sada P, Spencer J, Spitale J, Stewart S, Varsik J, Warell J, Wild W, Yanamandra-Fisher P, Fazio G, Hora J, Deutsch L. Earth-Based Observations of the Galileo Probe Entry Site. Science 1996; 272:839-40. [PMID: 8662571 DOI: 10.1126/science.272.5263.839] [Citation(s) in RCA: 51] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/01/2023]
Abstract
Earth-based observations of Jupiter indicate that the Galileo probe probably entered Jupiter's atmosphere just inside a region that has less cloud cover and drier conditions than more than 99 percent of the rest of the planet. The visual appearance of the clouds at the site was generally dark at longer wavelengths. The tropospheric and stratospheric temperature fields have a strong longitudinal wave structure that is expected to manifest itself in the vertical temperature profile.
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Affiliation(s)
- G Orton
- G. Orton, J. Friedson, T. Martin, P. Yanamandra-Fisher, Mail Stop 169-237, Jet Propulsion Laboratory (JPL), California Institute of Technology, Pasadena, CA 91109; J. L. Ortiz, Mail Stop 169-237, JPL, and Instituto de Astrofisica de Andalucia, CSIC, P.O. Box 3004, 18080 Granada, Spain; K. Baines, Mail Stop 183-601, JPL; G. Bjoraker, D. Deming, D. Jennings, G. McCabe, P. Sada, Code 693, NASA Goddard Space Flight Center, Greenbelt, MD 20771; U. Carsenty, DLR Institute for Planetary Exploration, Rudower Chaussee 5, D-12489 Berlin, Germany; F. Colas, Bureau des Longitudes, 75015 Paris, France; A. Dayal and W. Hoffmann, Stewart Observatory, Univ. of Arizona, Tucson, AZ 85721; P. Drossart and J. Lecacheux, DESPA, Observatoire de Paris-Meudon, 92195 Meudon Cedex, France; E. Frappa and P. Laques, Observatoire Midi-Pyrenees, 65200 Bagneres de Bigorre, France; J. Goguen, Mail Stop 183-501, JPL; W. Golisch, D. Griep, C. Kaminski, J. Hora, Institute for Astronomy, Univ. of Hawaii, Honolulu, HI 96822; C. Hernandez, 9430 S.W. 29 Terrace, Miami, FL 33165; J. Kuhn, H. Lin, J. Varsik, National Solar Observatory, Sunspot, NM 88349; S. Limaye, Space Science and Engineering Center, Univ. of Wisconsin, Madison, WI 53706; T. Momary, 3806 Geology Building, Univ. of California, Los Angeles, CA 90024-1567; D. Parker, 12911 Lerida Street, Coral Gables, FL 33156; R. Puetter, CASS, Univ. of California at San Diego, La Jolla, CA 92093-0111; M. Ressler, Mail Stop 169-506, JPL; G. Reyes, Mail Stop 300-329, JPL; J. Spencer, Lowell Observatory, 1400 Mars Hill Road, Flagstaff, AZ 86001; J. Spitale and S. Stewart, Division of Geological and Planetary Sciences, 170-20, California Institute of Technology, Pasadena, CA 91125; J. Warell, Uppsala Astronomical Observatory, Box 515, S-75120 Uppsala, Sweden; W. Wild, Department of Astronomy and Astrophysics, Univ. of Chicago, Chicago, IL 60637; G. Fazio, Smithsonian Astrophysical Observatory, Cambridge, MA 02138; L. Deutsch, Five College Astronomy Department, Univ. of Massachusetts, Amherst, MA 01003
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Chassefière E, Drossart P, Korablev O. Post-Phobos model for the altitude and size distribution of dust in the low Martian atmosphere. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je03363] [Citation(s) in RCA: 54] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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42
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Rosenqvist J, Drossart P, Combes M, Encrenaz T, Lellouch E, Bibring JP, Erard S, Langevin Y, Chassefiere E. Minor constituents in the Martian atmosphere from the ISM/Phobos experiment. Icarus 1992; 98:254-270. [PMID: 11539361 DOI: 10.1016/0019-1035(92)90094-n] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
Global Martian atmospheric results derived from the infrared imaging spectrometer ISM flown aboard the Phobos 2 Soviet spacecraft are presented. Over low altitude regions the expected CO mixing ratio of (8 +/- 3) x 10(-4) is measured. Variations of the 2.35-micrometers feature are inconsistent with this value over the Great Martian Volcanoes. If the 2.35-micrometers band is entirely attributable to carbon monoxide, the CO mixing ratio is typically depleted by a factor of 3 over these high altitude areas. Orography should play a major role in the existence of this CO "hole." If, however, these spectral variations at 2.35 micrometers are due to the surface composition, the fraction of the surface covered by the responsible mineral must smoothly decrease as the surface elevation decreases. This phenomenon implies a strong interaction between the surface and the atmosphere for the Great Martian Volcanoes. Diurnal behavior and latitudinal variations of water vapor are globally consistent with Viking measurements. During the Phobos observations, the water vapor amounts over the bright equatorial regions range around 11 pr-micrometers during the day. These amounts are slightly larger than those inferred from 1976 to 1979. The lack of global dust storms during 1988-1989 could explain the enhancement of H2O in the atmosphere.
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Affiliation(s)
- J Rosenqvist
- Departement de Recherches Spatiales, Observatoire de Paris-Meudon, France
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43
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Carlson RW, Baines KH, Encrenaz T, Taylor FW, Drossart P, Kamp LW, Pollack JB, Lellouch E, Collard AD, Calcutt SB, Grinspoon D, Weissman PR, Smythe WD, Ocampo AC, Danielson GE, Fanale FP, Johnson TV, Kieffer HH, Matson DL, McCord TB, Soderblom LA. Galileo Infrared Imaging Spectroscopy Measurements at Venus. Science 1991; 253:1541-8. [PMID: 17784099 DOI: 10.1126/science.253.5027.1541] [Citation(s) in RCA: 129] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
During the 1990 Galileo Venus flyby, the Near Infaied Mapping Spectrometer investigated the night-side atmosphere of Venus in the spectral range 0.7 to 5.2 micrometers. Multispectral images at high spatial resolution indicate substanmial cloud opacity variations in the lower cloud levels, centered at 50 kilometers altitude. Zonal and meridional winds were derived for this level and are consistent with motion of the upper branch of a Hadley cell. Northern and southern hemisphere clouds appear to be markedly different. Spectral profiles were used to derive lower atmosphere abundances of water vapor and other species.
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44
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Bibring JP, Combes M, Langevin Y, Soufflot A, Cara C, Drossart P, Encrenaz T, Erard S, Forni O, Gondet B, Ksanfomalfty L, Lellouch E, Masson P, Moroz V, Rocard F, Rosenqvist J, Sotin C. Results from the ISM experiment. Nature 1989. [DOI: 10.1038/341591a0] [Citation(s) in RCA: 103] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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