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1. Linking interstellar and cometary O$_2$: a deep search for $^{16}$O$^{18}$O in the solar-type protostar IRAS 16293--2422

Author

Taquet, Vianney, van Dishoeck, Ewine F., Swayne, Matthew, Harsono, Daniel, Jørgensen, Jes K., Maud, Luke, Ligterink, Niels F. W., Müller, Holger S. P., Codella, Claudio, Altwegg, Kathrin, Bieler, Andre, Coutens, Audrey, Drozdovskaya, Maria N., Furuya, Kenji, Persson, Magnus V., Hoff, Merel L. R. van 't, Walsh, Catherine, and Wampfler, Suzanne F.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Recent measurements carried out at comet 67P/C-G with the ${\it Rosetta}$ probe revealed that molecular oxygen, O$_2$, is the fourth most abundant molecule in comets. Models show that O$_2$ is likely of primordial nature, coming from the interstellar cloud from which our Solar System was formed. However, gaseous O$_2$ is an elusive molecule in the interstellar medium with only one detection towards quiescent molecular clouds, in the $\rho$ Oph A core. We perform a deep search for molecular oxygen, through the $2_1 - 0_1$ rotational transition at 234 GHz of its $^{16}$O$^{18}$O isotopologue, towards the warm compact gas surrounding the nearby Class 0 protostar IRAS 16293--2422 B with the ALMA interferometer. The targeted $^{16}$O$^{18}$O transition is surrounded by two brighter transitions at $\pm 1$ km s$^{-1}$ relative to the expected $^{16}$O$^{18}$O transition frequency. After subtraction of these two transitions, residual emission at a 3$\sigma$ level remains, but with a velocity offset of $0.3 - 0.5$ km s$^{-1}$ relative to the source velocity, rendering the detection "tentative". We derive the O$_2$ column density for two excitation temperatures $T_{\rm ex}$ of 125 and 300 K, as indicated by other molecules, in order to compare the O$_2$ abundance between IRAS16293 and comet 67P/C-G. Assuming that $^{16}$O$^{18}$O is not detected and using methanol CH$_3$OH as a reference species, we obtain a [O$_2$]/[CH$_3$OH] abundance ratio lower than $2-5$, depending on the assumed $T_{\rm ex}$, a three to four times lower abundance than the [O$_2$]/[CH$_3$OH] ratio of $5-15$ found in comet 67P/C-G. Such a low O$_2$ abundance could be explained by the lower temperature of the dense cloud precursor of IRAS16293 with respect to the one at the origin of our Solar System that prevented an efficient formation of O$_2$ in interstellar ices., Comment: 12 pages, 3 figures, accepted for publication in Astronomy & Astrophysics

Published
2018
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7. Prebiotic chemicals--amino acid and phosphorus--in the coma of comet 67P/Churyumov-Gerasimenko

Author

Altwegg, Kathrin, Balsiger, Hans, Bar-Nun, Akiva, Berthelier, Jean-Jacques, Bieler, Andre, Bochsler, Peter, Briois, Christelle, Calmonte, Ursina, Combi, Michael R., Cottin, Hervé, De Keyser, Johan, Dhooghe, Frederik, Fiethe, Bjorn, Fuselier, Stephen A., Gasc, Sébastien, Gombosi, Tamas I., Hansen, Kenneth C., Hässig, Myrtha, Jäckel, Annette, Kopp, Ernest, Korth, Axel, Le Roy, Léna, Mall, Urs, Marty, Bernard, Mousis, Olivier, Owen, Tobias, Rème, Henri, Rubin, Martin, Semon, Thierry, Tzou, Chia-yu, Hunter Waite, James, Wurz, Peter, 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), 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 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), 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), 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), State of Bern, Swiss National Science Foundation, ESA PRODEX (PROgramme de Développement d’Expériences scientifiques) program, Max Planck Society, Federal Ministry for Economic Affairs and Energy (BMWI), Jet Propulsion Laboratory (JPL), Belgian Science Policy Office, French National Re- search Agency (ANR), Centre National d'Etudes Spatiales (CNES, European Research Council, NASA, ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), European Project, Universität Bern [Bern], Department of Geosciences [Tel Aviv], Tel Aviv University [Tel Aviv], IMPEC - LATMOS, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Braunschweig [Braunschweig], Max-Planck-Institut für Sonnensystemforschung (MPS), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), ANR-11-IDEX-0001-02/11-IDEX-0001,AMIDEX,AMIDEX(2011), 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), 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), Center for Space and Habitability ( CSH ), 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 ), Laboratoire inter-universitaire des systèmes atmosphèriques ( LISA ), 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 ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), 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 ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), and Université de Lorraine (UL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
67P/Churyumov-Gerasimenko, animal structures, 530 Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry, complex mixtures, Mass Spectrometry, comets, Amino Acids, Research Articles, 520 Astronomy, prebiotic molecules, food and beverages, SciAdv r-articles, Phosphorus, Meteoroids, 620 Engineering, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], astronomy, Prebiotics, cardiovascular system, sense organs, Space Sciences, amino acid, Origins of life, Research Article
Abstract

The detection of glycine and phosphorus in the coma of 67P shows that comets contain all ingredients to help spark life on Earth., The importance of comets for the origin of life on Earth has been advocated for many decades. Amino acids are key ingredients in chemistry, leading to life as we know it. Many primitive meteorites contain amino acids, and it is generally believed that these are formed by aqueous alterations. In the collector aerogel and foil samples of the Stardust mission after the flyby at comet Wild 2, the simplest form of amino acids, glycine, has been found together with precursor molecules methylamine and ethylamine. Because of contamination issues of the samples, a cometary origin was deduced from the 13C isotopic signature. We report the presence of volatile glycine accompanied by methylamine and ethylamine in the coma of 67P/Churyumov-Gerasimenko measured by the ROSINA (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) mass spectrometer, confirming the Stardust results. Together with the detection of phosphorus and a multitude of organic molecules, this result demonstrates that comets could have played a crucial role in the emergence of life on Earth.

Published
2016

8. Highlights from the first year of Rosetta-ROSINA measurements at Comet 67P/Churyumov-Gerasimenko

Author

Bieler, Andre, Altwegg, Kathrin, Balsiger, Hans, Berthelier, Jean-Jacques, Johan De Keyser, Fuselier, Stephen, Gombosi, Tamas, Rubin, Martin, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Physikalisches Institut [Bern], Universität Bern [Bern], Center for Space and Habitability (CSH), University of Bern, 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), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Cardon, Catherine, and Universität Bern [Bern] (UNIBE)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The European Space Agency's Rosetta Mission arrived at Comet 67P/Churyumov-Gerasimenko in August 2014 and has been continuously conducting measurements of various aspects of the cometary environment ever since. In this talk we will present the most important findings from the first year of measurements with the ROSINA instrument suite, which is designed to characterize the volatile inventory of 67P. The high resolving power and sensitivity of the instruments allows to determine the composition of the coma even down to very rarified species. ROSINA has produced fundamental results necessary to better understand our own Solar System by the verification of the D/H ratio in cometary water, the detection of the noble gas Argon, and the confirmation / quantification of the presence of molecular Nitrogen in Jupiter family comets.

Published
2015

9. Solar wind sputtering of dust on the surface of 67P/Churyumov-Gerasimenko

Author

Wurz, Peter, Rubin, Martin, Altwegg, Kathrin, Balsiger, Hans, Berthelier, Jean-Jacques, Bieler, Andre, Calmonte, Ursina, Keyser, Johan, Fiethe, Bjoern, Fuselier, Stephen A., Galli, Andre, Gasc, Sebastien, Tamas Gombosi, Jaeckel, Annette, Le Roy, Lena, Mall, Urs A., Reme, Henri, Tenishey, Valeriy, Tzou, Chia-Yu, Center for Space and Habitability (CSH), University of Bern, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), 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, 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], The University of Texas at San Antonio (UTSA), 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, 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), Center for Space and Habitability ( CSH ), Universität Bern [Bern], 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 ), 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], The University of Texas at San Antonio ( UTSA ), Southwest Research Institute [San Antonio] ( SwRI ), Max Planck Institute for Solar System Research ( MPS ), 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 ), Max Planck Institute for Solar System Research (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), 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
Comet composition, 520 Astronomy, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Refractory material, 620 Engineering, Solar wind sputtering, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; Far away from the Sun, at around 3 AU, the activity of comet 67P/Churyumov-Gerasimenko is low and changes with local time (solar insolation), with location (chemical heterogeneity of the surface), and with season. When the activity is very low because the total cross section of the comet against the Sun is small, the solar wind has access to the surface of the comet and causes ion-induced sputtering of surface material, which we wish to observe.Methods. We used the Double Focussing Mass Spectrometer (DFMS) of the ROSINA experiment on ESA’s Rosetta mission to search for mass spectrometric evidence of sputtered refractory species. In high-resolution mode, DFMS can separate some of the mass peaks of refractory elements from the many volatile species present in the coma.Results. At present, the locations of solar wind surface access are in the southern hemisphere of the comet (the local winter). Of particular interest is sputtering of dust grains on the surface. We observe global averages over the winter hemisphere of the refractory elements Na, K, Si, and Ca, presumably sputtered from grains residing on the surface. Compared to carbonaceous chondrites, the comet has the same Na abundance, is depleted in Ca, and has an excess of K. In addition, for Si the signal strength is strong enough to compile a coarse compositional map of the southern hemisphere. Most, perhaps all, of the observed variation can be explained by the solar wind being affected by the atmosphere of the comet.

Published
2015

11. A 3D Description of the Coma of Comet 67P/Churyumov-Gerasimenko Constrained by Rosetta Observations

Author

Fougere, Nicolas, Tenishev, Valeriy, Bieler, Andre, Combi, Michael, Gombosi, Tamas, Hansen, Kenneth, Jia, Xianzhe, Shou, Yinsi, Huang, Zhenguang, Toth, Gabor, Altwegg, Kathrin, Wurz, Peter, Balsiger, Hans, Jäckel, Annette, Le Roy, Lena, Gasc, Sébastien, Calmonte, Ursina, Rubin, Martin, Tzou, Chia-Yu, Hässig, Myrtha, Fuselier, Stephen, Johan De Keyser, Berthelier, Jean-Jacques, Mall, Urs, Rème, Henri, Fiethe, Björn, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), University of Michigan [Ann Arbor], Physikalisches Institut [Bern], Universität Bern [Bern], Space Science Division [San Antonio], Southwest Research Institute [San Antonio] ( SwRI ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), 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 ), Max Planck Institute for Solar System Research ( MPS ), 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 ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan System-University of Michigan System, Southwest Research Institute [San Antonio] (SwRI), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Institut de recherche en astrophysique et planétologie (IRAP), 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), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), and 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)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; For the first time, the Rosetta spacecraft stays with a comet over an extended period of time during its journey in the inner the solar system. The data provided by the suite of instruments on board the Rosetta spacecraft, notably the ROSINA mass spectrometers and the pressure sensor, provides critical information concerning comet 67P/Churyumov-Gerasimenko (CG) and its environment. These measurements reinforce our knowledge of comet CG and enable us to describe the nucleus and the sources with more details. The observations allow us to better constrain and accordingly develop much more realistic models of the comet’s coma.We show a 3D simulation of the gas and dust coma of comet CG using a Direct Simulation Monte-Carlo model performed with the Adaptive Mesh Particle Simulator (Tenishev et al. 2008, 2011). The coma model presented includes a realistic nucleus shape, with a gas flux distribution and a surface temperature that takes into account irregularities and concavities of the nucleus. Along with the gas drag, the gravity field drives the dust dynamics and is therefore accurately computed around the irregular nucleus shape. This constitutes the state-of-the-art of cometary coma models, which are crucial to interpret instrument data and for further mission planning.Acknowledgement:This work was supported by contracts JPL#1266313 and JPL#1266314 from the US Rosetta Project and NASA grant NNX09AB59G from the Planetary Atmospheres Program.References:Tenishev et al. 2008 ApJ 685:659, and 2011 ApJ 732:104

Published
2014

12. 3D Direct Simulation Monte Carlo Modeling of the Spacecraft Environment of Rosetta

Author

Bieler, Andre, Tenishev, Valeriy, Fougere, Nicolas, Gombosi, Tamas, Hansen, Kenneth, Combi, Michael, Huang, Zhenguang, Jia, Xianzhe, Toth, Gabor, Altwegg, Kathrin, Wurz, Peter, Jäckel, Annette, Le Roy, Lena, Gasc, Sébastien, Calmonte, Ursina, Rubin, Martin, Tzou, Chia-Yu, Hässig, Myrtha, Fuselier, Stephen, Johan De Keyser, Berthelier, Jean-Jacques, Mall, Urs, Rème, Henri, Fiethe, Björn, Balsiger, Hans, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Physikalisches Institut [Bern], Universität Bern [Bern], Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Institut de recherche en astrophysique et planétologie (IRAP), 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), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Southwest Research Institute [San Antonio] ( SwRI ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), 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 ), Max Planck Institute for Solar System Research ( MPS ), 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 ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), and 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)

Subjects
Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::Earth and Planetary Astrophysics, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The European Space Agency’s Rosetta mission is the first to escort a comet over an extended time as the comet makes its way through the inner solar system. The ROSINA instrument suite consisting of a double focusing mass spectrometer, a time of flight mass spectrometer and a pressure sensor, will provide temporally and spatially resolved data on the comet’s volatile inventory.The effect of spacecraft outgassing is well known and has been measured with the ROSINA instruments onboard Rosetta throughout the cruise phase. The flux of released neutral gas originating from the spacecraft cannot be distinguished from the cometary signal by the mass spectrometers and varies significantly with solar illumination conditions. For accurate interpretation of the instrument data, a good understanding of spacecraft outgassing is necessary. In this talk we present results simulating the spacecraft environment with the Adaptive Mesh Particle Simulator (AMPS) code. AMPS is a direct simulation monte carlo code that includes multiple species in a 3D adaptive mesh to describe a full scale model of the spacecraft environment. We use the triangulated surface model of the spacecraft to implement realistic outgassing rates for different areas on the surface and take shadowing effects in consideration. The resulting particle fluxes are compared to the measurements of the ROSINA experiment and implications for ROSINA measurements and data analysis are discussed. Spacecraft outgassing has implications for future space missions to rarefied atmospheres as it imposes a limit on the detection of various species.

Published
2014

13. Cometary Nitrogen-Noble gases and the Origin of the Oceans: Waiting for ROSINA-Rosetta Data (invited)

Author

Marty, Bernard, Calmonte, Ursina, Altwegg, Kathrin, Balsiger, Hans, Bar-Nun, Akiva, Berthelier, Jean-Jacques, Bieler, Andre, Dhooghe, Frederik, Fiethe, Björn, Mall, Urs, Mousis, Olivier, Owen, Tobias, Rubin, Martin, Centre de Recherches Pétrographiques et Géochimiques (CRPG), Université de Lorraine (UL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Physikalisches Institut [Bern], Universität Bern [Bern], Department of Geosciences [Tel Aviv], Tel Aviv University [Tel Aviv], 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, 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], 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 national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern] (UNIBE), Department of Geophysics [Tel Aviv] (TAU), Tel Aviv University (TAU), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Cardon, Catherine, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The origin of the terrestrial oceans and atmosphere is still a matter of intensive debate. For a while high D/H ratios in comets compared to both meteorites and Earth’s oceans (which share approximately the same range of values) has been taken as evidence for an asteroidal origin of the oceans. This possibility is in line with the N isotope composition of meteorites encompassing the terrestrial atmosphere value. Recently, Earth-like D/H ratios have been reported for two comets, thus re-vitalizing the possibility of cometary contribution to terrestrial volatiles. Nitrogen in cometary CN, HCN, and NH2 (the N-bearing molecules that can be analyzed remotely) is enriched by a factor of approx. 80% in 15N compared to terrestrial N. The question is whether or not these N-bearing molecules are representative of bulk N in comets. If nitrogen is trapped as N2 in cometary ices, its isotope composition could reflect that of the protosolar nebula, which was depleted by 40% relative to Earth. A cometary cocktail consisting of 1/3 reduced, 15N-rich N and 2/3 of nebula-like N2 would make the terrestrial N isotope composition. Another strong constraint will arise from the analysis of cometary noble gases which, if trapped at sufficiently low temperature in ice, could account for the elevated noble gas/H,C ratio of the terrestrial surface reservoirs. Hopefully, the ROSINA instrument on board of the Rosetta spacecraft which will analyze volatile elements degassed by comet 67/P Churyumov-Gerasimenko, which should permit to shed light on this fundamental issue.

Published
2014

14. Four‐fluid MHD simulations of the plasma and neutral gas environment of comet 67P/Churyumov‐Gerasimenko near perihelion

Author

Huang, Zhenguang, primary, Tóth, Gábor, additional, Gombosi, Tamas I., additional, Jia, Xianzhe, additional, Rubin, Martin, additional, Fougere, Nicolas, additional, Tenishev, Valeriy, additional, Combi, Michael R., additional, Bieler, Andre, additional, Hansen, Kenneth C., additional, Shou, Yinsi, additional, and Altwegg, Kathrin, additional

Published
2016
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15. Comparison of 3D kinetic and hydrodynamic models to ROSINA-COPS measurements of the neutral coma of 67P/Churyumov-Gerasimenko

Author

Bieler, Andre, primary, Altwegg, Kathrin, additional, Balsiger, Hans, additional, Berthelier, Jean-Jacques, additional, Calmonte, Ursina, additional, Combi, Michael, additional, De Keyser, Johan, additional, Fiethe, Björn, additional, Fougere, Nicolas, additional, Fuselier, Stephen, additional, Gasc, Sébastien, additional, Gombosi, Tamas, additional, Hansen, Kenneth, additional, Hässig, Myrtha, additional, Huang, Zhenguang, additional, Jäckel, Annette, additional, Jia, Xianzhe, additional, Le Roy, Lena, additional, Mall, Urs A., additional, Rème, Henri, additional, Rubin, Martin, additional, Tenishev, Valeriy, additional, Tóth, Gábor, additional, Tzou, Chia-Yu, additional, and Wurz, Peter, additional

Published
2015
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16. Inventory of the volatiles on comet 67P/Churyumov-Gerasimenko from Rosetta/ROSINA

Author

Le Roy, Léna, primary, Altwegg, Kathrin, additional, Balsiger, Hans, additional, Berthelier, Jean-Jacques, additional, Bieler, Andre, additional, Briois, Christelle, additional, Calmonte, Ursina, additional, Combi, Michael R., additional, De Keyser, Johan, additional, Dhooghe, Frederik, additional, Fiethe, Björn, additional, Fuselier, Stephen A., additional, Gasc, Sébastien, additional, Gombosi, Tamas I., additional, Hässig, Myrtha, additional, Jäckel, Annette, additional, Rubin, Martin, additional, and Tzou, Chia-Yu, additional

Published
2015
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17. Detection of argon in the coma of comet 67P/Churyumov-Gerasimenko

Author

Balsiger, Hans, primary, Altwegg, Kathrin, additional, Bar-Nun, Akiva, additional, Berthelier, Jean-Jacques, additional, Bieler, Andre, additional, Bochsler, Peter, additional, Briois, Christelle, additional, Calmonte, Ursina, additional, Combi, Michael, additional, De Keyser, Johan, additional, Eberhardt, Peter, additional, Fiethe, Björn, additional, Fuselier, Stephen A., additional, Gasc, Sébastien, additional, Gombosi, Tamas I., additional, Hansen, Kenneth C., additional, Hässig, Myrtha, additional, Jäckel, Annette, additional, Kopp, Ernest, additional, Korth, Axel, additional, Le Roy, Lena, additional, Mall, Urs, additional, Marty, Bernard, additional, Mousis, Olivier, additional, Owen, Tobias, additional, Rème, Henri, additional, Rubin, Martin, additional, Sémon, Thierry, additional, Tzou, Chia-Yu, additional, Waite, J. Hunter, additional, and Wurz, Peter, additional

Published
2015
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19. Contributors

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

20. Index

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

22. Back Cover

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

34. Acronyms and Abbreviations

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

36. Acknowledgements

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

37. Tables and Figures

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

38. Front Cover

Author

Satgar, Vishwas, Carroll, William K, Hunt-Hendrix, Leah, Christie, Isham, Bieler, Andreas, and Jordan, Jamie

Published
2010

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