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49 results on '"Engrand, Cécile"'

1. Variations of organic functional chemistry in carbonaceous matter from the asteroid 162173 Ryugu

Author

De Gregorio, Bradley, Cody, George D., Stroud, Rhonda M., David Kilcoyne, A. L., Sandford, Scott, Le Guillou, Corentin, Nittler, Larry R., Barosch, Jens, Yabuta, Hikaru, Martins, Zita, Kebukawa, Yoko, Okumura, Taiga, Hashiguchi, Minako, Yamashita, Shohei, Takeichi, Yasuo, Takahashi, Yoshio, Wakabayashi, Daisuke, Engrand, Cécile, Bejach, Laure, Bonal, Lydie, Quirico, Eric, Remusat, Laurent, Duprat, Jean, Verdier-Paoletti, Maximilien, Mostefaoui, Smail, Komatsu, Mutsumi, Mathurin, Jérémie, Dazzi, Alexandre, Deniset-Besseau, Ariane, Dartois, Emmanuel, Tamenori, Yusuke, Suga, Hiroki, Montagnac, Gilles, Kamide, Kanami, Shigenaka, Miho, Matsumoto, Megumi, Enokido, Yuma, Yoshikawa, Makoto, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Nakazawa, Satoru, Usui, Tomohiro, Abe, Masanao, Okada, Tatsuaki, Yada, Toru, Nishimura, Masahiro, Nakato, Aiko, Miyazaki, Akiko, Yogata, Kasumi, Yurimoto, Hisayoshi, Nakamura, Tomoki, Noguchi, Takaaki, Okazaki, Ryuji, Naraoka, Hiroshi, Sakamoto, Kanako, Tachibana, Shogo, Watanabe, Sei-ichiro, and Tsuda, Yuichi

Published
2024
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2. The thermal history of Ryugu based on Raman characterization of Hayabusa2 samples

Author

Bonal, Lydie, Quirico, Eric, Montagnac, Gilles, Komatsu, Mutsumi, Kebukawa, Yoko, Yabuta, Hikaru, Amano, Kana, Barosch, Jens, Bejach, Laure, Cody, George D., Dartois, Emmanuel, Dazzi, Alexandre, De Gregorio, Bradley, Deniset-Besseau, Ariane, Duprat, Jean, Engrand, Cécile, Hashiguchi, Minako, Kamide, Kanami, Kilcoyne, David, Martins, Zita, Mathurin, Jérémie, Mostefaoui, Smail, Nittler, Larry, Ohigashi, Takuji, Okumura, Taiga, Remusat, Laurent, Sandford, Scott, Shigenaka, Miho, Stroud, Rhonda, Suga, Hiroki, Takahashi, Yoshio, Takeichi, Yasuo, Tamenori, Yusuke, Verdier-Paoletti, Maximilien, Yamashita, Shohei, Nakamura, Tomoki, Naraoka, Hiroshi, Noguchi, Takaaki, Okazaki, Ryuji, Yurimoto, Hisayoshi, Tachibana, Shogo, Abe, Masanao, Miyazaki, Akiko, Nakato, Aiko, Nakazawa, Satoru, Nishimura, Masahiro, Okada, Tatsuaki, Saiki, Takanao, Sakamoto, Kanako, Tanaka, Satoshi, Terui, Fuyuto, Tsuda, Yuichi, Usui, Tomohiro, Watanabe, Sei-ichiro, Yada, Toru, Yogata, Kasumi, and Yoshikawa, Makota

Published
2024
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3. On structural properties of Comet 67/P dust particles collected in situ by ROSETTA/COSIMA from observations of electrical fragmentation

Author

Hornung, Klaus, Mellado, Eva Maria, Stenzel, Oliver J., Langevin, Yves, Merouane, Sihane, Fray, Nicolas, Fischer, Henning, Paquette, John, Baklouti, Donia, Bardyn, Anais, Engrand, Cecile, Cottin, Hervé, Thirkell, Laurent, Briois, Christelle, Rynö, Jouni, Silen, Johan, Schulz, Rita, Siljeström, Sandra, Lehto, Harry, Varmuza, Kurt, Koch, Andreas, Kissel, Jochen, and Hilchenbach, Martin

Published
2023
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4. AMBITION – comet nucleus cryogenic sample return

Author

Bockelée-Morvan, D., Filacchione, Gianrico, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Choukroun, Mathieu, Codella, Claudio, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria Cristina, Drozdovskaya, Maria N., Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Herique, Alain, Ivanovski, Stavro, Kokotanekova, Rosita, Levasseur-Regourd, Anny-Chantal, Miller, Kelly E., Rotundi, Alessandra, Schönbächler, Maria, Snodgrass, Colin, Thomas, Nicolas, Tubiana, Cecilia, Ulamec, Stephan, and Vincent, Jean-Baptiste

Published
2022
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5. Complex mixture of organic matter in a xenolithic clast from the Zag meteorite revealed by coordinated analyses using AFM-IR, NanoSIMS and STXM/XANES

Author

Kebukawa, Yoko, Mathurin, Jérémie, Dartois, Emmanuel, Dazzi, Alexandre, Deniset-Besseau, Ariane, Duprat, Jean, Remusat, Laurent, Noguchi, Takaaki, Miyake, Akira, Igami, Yohei, Paoletti, Maximilien Verdier, Zolensky, Michael E., Engrand, Cécile, Sandt, Christophe, Borondics, Ferenc, Yamashita, Shohei, Wakabayashi, Daisuke, Takeichi, Yasuo, and Takahashi, Yoshio

Published
2023
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6. Heterogeneous nature of the carbonaceous chondrite breccia Aguas Zarcas – Cosmochemical characterization and origin of new carbonaceous chondrite lithologies

Author

Kerraouch, Imene, Kebukawa, Yoko, Bischoff, Addi, Zolensky, Michael E., Wölfer, Elias, Hellmann, Jan L., Ito, Motoo, King, Ashley, Trieloff, Mario, Barrat, Jean-Alix, Schmitt-Kopplin, Phillipe, Pack, Andreas, Patzek, Markus, Hanna, Romy D., Fockenberg, Thomas, Marrocchi, Yves, Fries, Marc, Mathurin, Jérémie, Dartois, Emmanuel, Duprat, Jean, Engrand, Cécile, Deniset, Ariane, Dazzi, Alexandre, Kiryu, Kento, Igisu, Motoko, Shibuya, Takazo, Wakabayashi, Daisuke, Yamashita, Shohei, Takeichi, Yasuo, Takahashi, Yoshio, Ohigashi, Takuji, Kodama, Yu, and Kondo, Masashi

Published
2022
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8. Electrical properties of cometary dust particles derived from line shapes of TOF-SIMS spectra measured by the ROSETTA/COSIMA instrument

Author

Hornung, Klaus, Mellado, Eva Maria, Paquette, John, Fray, Nicolas, Fischer, Henning, Stenzel, Oliver, Baklouti, Donia, Merouane, Sihane, Langevin, Yves, Bardyn, Anais, Engrand, Cecile, Cottin, Hervé, Thirkell, Laurent, Briois, Christelle, Modica, Paola, Rynö, Jouni, Silen, Johan, Schulz, Rita, Siljeström, Sandra, Lehto, Harry, Varmuza, Kurt, Koch, Andreas, Kissel, Jochen, and Hilchenbach, Martin

Published
2020
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9. Microscale hydrogen, carbon, and nitrogen isotopic diversity of organic matter in asteroid Ryugu

Author

Nittler, Larry R, Barosch, Jens, Burgess, Katherine, Stroud, Rhonda M, Wang, Jianhua, Yabuta, Hikaru, Enokido, Yuma, Matsumoto, Megumi, Nakamura, Tomoki, Kebukawa, Yoko, Yamashita, Shohei, Takahashi, Yoshio, Bejach, Laure, Bonal, Lydie, Cody, George D, Dartois, Emmanuel, Dazzi, Alexandre, De Gregorio, Bradley, Deniset-Besseau, Ariane, Duprat, Jean, Engrand, Cécile, Hashiguchi, Minako, Kilcoyne, A.L. David, Komatsu, Mutsumi, Martins, Zita, Mathurin, Jérémie, Montagnac, Gilles, Mostefaoui, Smail, Okumura, Taiga, Quirico, Eric, Remusat, Laurent, Sandford, Scott, Shigenaka, Miho, Suga, Hiroki, Takeichi, Yasuo, Tamenori, Yusuke, Verdier-Paoletti, Maximilien, Wakabayashi, Daisuke, Abe, Masanao, Kamide, Kanami, Miyazaki, Akiko, Nakato, Aiko, Nakazawa, Satoru, Nishimura, Masahiro, Okada, Tatsuaki, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Usui, Tomohiro, Yada, Toru, Yogata, Kasumi, Yoshikawa, Makoto, Yurimoto, Hisayoshi, Noguchi, Takaaki, Okazaki, Ryuji, Naraoka, Hiroshi, Sakamoto, Kanako, Tachibana, Shogo, Watanabe, Sei-ichiro, and Tsuda, Yuichi

Published
2024
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11. Mechanical and electrostatic experiments with dust particles collected in the inner coma of comet 67P by COSIMA onboard Rosetta

Author

Hilchenbach, Martin, Fischer, Henning, Langevin, Yves, Merouane, Sihane, Paquette, John, Rynö, Jouni, Stenzel, Oliver, Briois, Christelle, Kissel, Jochen, Koch, Andreas, Schulz, Rita, Silen, Johan, Altobelli, Nicolas, Baklouti, Donia, Bardyn, Anais, Cottin, Herve, Engrand, Cecile, Fray, Nicolas, Haerendel, Gerhard, Henkel, Hartmut, Höfner, Herwig, Hornung, Klaus, Lehto, Harry, Mellado, Eva Maria, Modica, Paola, Le Roy, Lena, Siljeström, Sandra, Steiger, Wolfgang, Thirkell, Laurent, Thomas, Roger, Torkar, Klaus, Varmuza, Kurt, and Zaprudin, Boris

Published
2017

16. Cometary Dust

Author

Levasseur-Regourd, Anny-Chantal, Agarwal, Jessica, Cottin, Hervé, Engrand, Cécile, Flynn, George, Fulle, Marco, Gombosi, Tamas, Langevin, Yves, Lasue, Jérémie, Mannel, Thurid, Merouane, Sihane, Poch, Olivier, Thomas, Nicolas, and Westphal, Andrew

Published
2018
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17. Cometary Isotopic Measurements

Author

Bockelée-Morvan, Dominique, Calmonte, Ursina, Charnley, Steven, Duprat, Jean, Engrand, Cécile, Gicquel, Adeline, Hässig, Myrtha, Jehin, Emmanuël, Kawakita, Hideyo, Marty, Bernard, Milam, Stefanie, Morse, Andrew, Rousselot, Philippe, Sheridan, Simon, and Wirström, Eva

Published
2015
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18. Chemical composition of carbonaceous asteroid Ryugu from synchrotron spectroscopy in the mid- to far-infrared of Hayabusa2-returned samples.

Author

Dartois, Emmanuel, Kebukawa, Yoko, Yabuta, Hikaru, Mathurin, Jérémie, Engrand, Cécile, Duprat, Jean, Bejach, Laure, Dazzi, Alexandre, Deniset-Besseau, Ariane, Bonal, Lydie, Quirico, Eric, Sandt, Christophe, Borondics, Ferenc, Barosch, Jens, Cody, George D., De Gregorio, Brad T., Hashiguchi, Minako, Kilcoyne, David A. L., Komatsu, Mutsumi, and Martins, Zita

Subjects
ASTEROIDS, SOLAR system, SYNCHROTRONS, SAPONITE, SMALL solar system bodies, CHONDRITES
Abstract

Context. The current period is conducive to exploring our Solar System's origins with recent and future space sample return missions, which provide invaluable information from known Solar System asteroids and comets The Hayabusa2 mission of the Japan Aerospace Exploration Agency (JAXA) recently brought back samples from the surface of the Ryugu carbonaceous asteroid. Aims. We aim to identify the different forms of chemical composition of organic matter and minerals that constitute these Solar System primitive objects, to shed light on the Solar System's origins. Methods. In this work, we recorded infrared (IR) hyper-spectral maps of whole-rock Ryugu asteroid samples at the highest achievable spatial resolution with a synchrotron in the mid-IR (MIR). Additional global far-IR (FIR) spectra of each sample were also acquired. Results. The hyper-spectral maps reveal the variability of the functional groups at small scales and the intimate association of phyl-losilicates with the aliphatic components of the organic matter present in Ryugu. The relative proportion of column densities of the identified IR functional groups (aliphatics, hydroxyl + interlayer and/or physisorbed water, carbonyl, carbonates, and silicates) giving access to the composition of the Ryugu samples is estimated from these IR hyper-spectral maps. Phyllosilicate spectra reveal the presence of mixtures of serpentine and saponite. We do not detect anhydrous silicates in the samples analysed, at the scales probed. The carbonates are dominated by dolomite. Aliphatics organics are distributed over the whole samples at the micron scale probed with the synchrotron, and intimately mixed with the phyllosilicates. The aromatic C=C contribution could not be safely deconvolved from OH in most spectra, due to the ubiquitous presence of hydrated minerals. The peak intensity ratios of the organics methylene to methyl (CH2/CH3) of the Ryugu samples vary between about 1.5 and 2.5, and are compared to the ratios in chondrites from types 1 to 3. Overall, the mineralogical and organic characteristics of the Ryugu samples show similarities with those of CI chondrites, although with a noticeably higher CH2/CH3 in Ryugu than generally measured in C1 chondrites collected on Earth, and possibly a higher carbonate content. [ABSTRACT FROM AUTHOR]

Published
2023
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19. Presolar Stardust in Asteroid Ryugu

Author

Barosch, Jens, Nittler, Larry R., Wang, Jianhua, Alexander, Conel M.O’D., De Gregorio, Bradley T., Engrand, Cécile, Kebukawa, Yoko, Nagashima, Kazuhide, Stroud, Rhonda M., Yabuta, Hikaru, Abe, Yoshinari, Aléon, Jérôme, Amari, Sachiko, Amelin, Yuri, Bajo, Ken-ichi, Bejach, Laure, Bizzarro, Martin, Bonal, Lydie, Bouvier, Audrey, Carlson, Richard W., and Schönbächler, Maria

Abstract

We have conducted a NanoSIMS-based search for presolar material in samples recently returned from C-type asteroid Ryugu as part of JAXA's Hayabusa2 mission. We report the detection of all major presolar grain types with O- and C-anomalous isotopic compositions typically identified in carbonaceous chondrite meteorites: 1 silicate, 1 oxide, 1 O-anomalous supernova grain of ambiguous phase, 38 SiC, and 16 carbonaceous grains. At least two of the carbonaceous grains are presolar graphites, whereas several grains with moderate C isotopic anomalies are probably organics. The presolar silicate was located in a clast with a less altered lithology than the typical extensively aqueously altered Ryugu matrix. The matrix-normalized presolar grain abundances in Ryugu are ${4.8}_{-2.6}^{+4.7}$ ppm for O-anomalous grains, ${25}_{-5}^{+6}$ ppm for SiC grains, and ${11}_{-3}^{+5}$ ppm for carbonaceous grains. Ryugu is isotopically and petrologically similar to carbonaceous Ivuna-type (CI) chondrites. To compare the in situ presolar grain abundances of Ryugu with CI chondrites, we also mapped Ivuna and Orgueil samples and found a total of 15 SiC grains and 6 carbonaceous grains. No O-anomalous grains were detected. The matrix-normalized presolar grain abundances in the CI chondrites are similar to those in Ryugu: ${23}_{-6}^{+7}$ ppm SiC and ${9.0}_{-3.6}^{+5.4}$ ppm carbonaceous grains. Thus, our results provide further evidence in support of the Ryugu–CI connection. They also reveal intriguing hints of small-scale heterogeneities in the Ryugu samples, such as locally distinct degrees of alteration that allowed the preservation of delicate presolar material., The Astrophysical Journal Letters, 935 (1), ISSN:1967-2014, ISSN:2041-8213

Published
2022
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22. AMBITION, the Comet Nucleus Cryogenic Sample Return mission for ESA Voyage 2050 program

Author

Filacchione, Gianrico, Bockelée-Morvan, Dominique, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Codella, Claudio, Choukroun, Mathieu, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria Cristina, Drozdovskaya, Maria, Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Hérique, Alain, Ivanovski, Stavro L., Kokotanekova, Rosita, Levasseur-Regourd, Anny Chantal, Miller, Kelly E., Rotundi, Alessandra, Schönbächler, Maria, Snodgrass, Colin, Thomas, Nicolas, Tubiana, Cécilia, Ulamec, Stefan, Vincent, Jean-Baptiste, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Centre for Star and Planet Formation (STARPLAN), Globe Institute, Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], INAF - Osservatorio Astrofisico di Arcetri (OAA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Center for Space and Habitability (CSH), University of Bern, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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), INAF - Osservatorio Astronomico di Trieste (OAT), European Southern Observatory [Garching], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [San Antonio] (SwRI), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Cardon, Catherine, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universität Bern [Bern], Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), California Institute of Technology (CALTECH)-NASA, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2020

26. Fragments from the Origins of the Solar System and our Interstellar Locale (FOSSIL): A Discovery Mission Concept

Author

Horanyi, Mihaly, Turner, Neal J., Alexander, Conel M. O'D., Altobelli, Nicolas, Balint, Tibor S., Castillo-Rogez, Julie, Draine, Bruce, Engrand, Cécile, Hillier, Jon K., Ishii, Hope, Kempf, Sascha, Munsat, Tobin, Nesvorny, David, Nittler, L. R., Pokorný, Peter, Postberg, Frank, Srama, Ralf, Stephan, Thomas, Sternovsky, Zoltan, Szalay, James, Westphal, Andrew J., Wooden, Diane, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], European Space Astronomy Centre (ESAC), European Space Agency (ESA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), University of Kent [Canterbury], and Engrand, Cecile

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019

27. AMBITION Comet Nucleus Cryogenic Sample Return

Author

Bockelée-Morvan, D., Filacchione, Gianrico, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Codella, Claudio, Choukroun, Mathieu, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria Cristina, Drozdovskaya, Maria, Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Herique, Alain, Ivanoski, Stavro, Kokotanekova, Rosita, Levasseur-Regourd, Anny Chantal, Miller, Kelly E., Rotundi, Alessandra, Schönbächler, Maria, Snodgrass, Colin, Thomas, Nicolas, Tubiana, Cecilia, Ulamec, Stefan, Vincent, Jean-Baptiste, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Physikalisches Institut [Bern], Universität Bern [Bern], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre for Star and Planet Formation (STARPLAN), Globe Institute, Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Natural History Museum of Denmark, Faculty of Science [Copenhagen], Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig [Braunschweig], INAF - Osservatorio Astrofisico di Arcetri (OAA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), 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), Center for Space and Habitability (CSH), University of Bern, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Department of Physics [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, 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)-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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), European Southern Observatory (ESO), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [San Antonio] (SwRI), Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [SDU]Sciences of the Universe [physics], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

This white paper proposes that AMBITION, a Comet Nucleus Sample Return mission, be a cornerstone of ESA's Voyage 2050 programme. We summarise some of the most important questions still open in cometary science after the successes of the Rosetta mission, many of which require sample analysis using techniques that are only possible in laboratories on Earth. We then summarise measurements, instrumentation and mission scenarios that can address these questions, with a recommendation that ESA select an ambitious cryogenic sample return mission. Rendezvous missions to Main Belt comets and Centaurs are compelling cases for M-class missions, expanding our knowledge by exploring new classes of comets. AMBITION would engage a wide community, drawing expertise from a vast range of disciplines within planetary science and astrophysics. With AMBITION, Europe will continue its leadership in the exploration of the most primitive Solar System bodies., 8 figures, 26 pages

Published
2019

28. Cometary dust: structure at the nanometre scale

Author

Mannel, Thurid, Bentley, Mark, Boakes, Peter, Jeszenszky, Harald, Ehrenfreund, Pascale, Engrand, Cécile, Koeberl, Christian, Levasseur-Regourd, Anny Chantal, Romstedt, Jens, Schmied, Roland, Torkar, Klaus, Weber, Iris, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Karl-Franzens-Universität Graz, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Leiden Observatory [Leiden], Universiteit Leiden, Space Policy Institute [Washington], The George Washington University (GW), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Lithospheric Research [Wien], Universität Wien, Natural History Museum [Vienna] (NHM), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Institut für Weltraumforschung = Space Research institute [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Karl-Franzens-Universität [Graz, Autriche], European Space Agency (ESA), Universiteit Leiden [Leiden], Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut für Weltraumforschung [Graz] (IWF), Westfälische Wilhelms-Universität Münster (WWU), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Rosetta orbiter carried three dedicated dust analysis instruments to investigate the properties of the comet andits dust at smallest scales. The images with the highest resolutions were obtained by the MIDAS (Micro-ImagingDust Analysis System) atomic force microscope [1,2]. It collected dust particles of one to tens of micrometresin size and imaged their surface in 3D. Nominal images had approximately hundreds of nanometres resolutionand were used to study the particle morphology at the micrometre scale. It was shown that the majority ofcollected particles were fragile agglomerates [3] with a moderate packing density of subunits at the surface [4].Exceptions were one extremely porous particle with a fractal structure that is suggested to be pristinely preservedfrom early agglomeration processes in our Solar System [4], and the particles of about one micrometre size thatshow less fragility. To study these smallest detected particles a special scanning mode, called ‘reverse imagingmode‘, was developed that reached resolutions down to eight nanometres [5]. In the reverse imaging mode dustparticles were picked up with the tip and imaged with the help of a sharp spike on a calibration sample. Theresulting images opened the possibility to identify the agglomerate structure of the dust down to the nanometrescale and to determine smallest features with mean sizes of about 100 nanometres. Whether these smallestfeatures are surface related or true subunits comprising the dust will be discussed on the basis of comparisons tosmallest subunit sizes identified by indirect Rosetta measurements and by investigations of other cometary material.References:[1] W. Riedler, K. Torkar, H. Jeszenszky, et al., MIDAS – The Micro-Imaging Dust Analysis System for theRosetta Mission. Space Science Reviews 128, 2007.[2] M.S. Bentley, H. Arends, B. Butler, et al., MIDAS: Lessons learned from the first spaceborne atomic forcemicroscope. Acta Astronautica 125, 2016.[3] M.S. Bentley, R. Schmied, T. Mannel et al., Aggregate dust particles at comet 67P/Chruyumov-Gerasimenko,Nature, 537, 2016.[4] T. Mannel, M.S. Bentley, R. Schmied et al., Fractal cometary dust – a window into the early Solar system,MNRAS, 462, 2016.[5] T. Mannel, M.S. Bentley, P.D. Boakes, et al., MIDAS results: classification and extension to the nanometrescale, submitted to Astronomy & Astrophysics, Rosetta special issue, 2018.

Published
2019

29. The Post-Rosetta Understanding of the Fate of Cometary Dust

Author

Levasseur-Regourd, Anny Chantal, Bentley, Mark, Cottin, Hervé, Engrand, Cécile, Freissinet, Caroline, Hadamcik, Edith, Langevin, Yves, Lasue, Jérémie, Mannel, Thurid, Merouane, Sihane, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), 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), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Cardon, Catherine, IMPEC - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and 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)

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

International audience; Thanks to its long duration, the Rosetta mission has provided a unique insight into the properties of dust particles released by 67P/C-G nucleus, and ascertained the links between cometary dust and CP-IDPs or UCAMMs [1]. Minerals to organics proportions are quite comparable within the refractory phase, in which carbon-bearing compounds present high-molecular masses [2-4]. Dust particles consist of aggregates of smaller grains and present hierarchical structures, with morphologies ranging from extremely porous to almost compact [5-7].The refractory materials released in comae (monitored with ≈ 4-1.2 au solar distance range for 67P/C-G), subjected to gravitational and non-gravitational forces, build up dust tails and trails, and progressively become parts of the zodiacal cloud, i.e. the lenticular-shaped interplanetary dust cloud. The small dust particles spiral towards the Sun under Poynting-Robertson effect, with migration times in the 300-50000 years range for micron-sized grains with densities about 100-1000 kg m-3 released at solar distances about 4-1.2 au [8]. Such dust particles happen to encounter the Earth atmosphere. Independent approaches have established that most of the near-Earth interplanetary dust comes from Jupiter Family comets, such as 67P/C-G [9-11], which orbit in the vicinity of the ecliptic plane.Updates of our present understanding of dust in 67P/C-G will be proposed. Through various numerical and experimental simulations [e.g. 12], the changes in composition and in physical properties of cometary dust particles in the interplanetary dust cloud will be discussed, as a function of time and of solar distance. The possible implications, for the early evolution of terrestrial planets, of the properties of the cometary dust component in the interplanetary dust cloud will be tentatively addressed.1. Levasseur-Regourd et al. SSR 2018. 2. Goesmann et al. Science 2015. 3. Fray et al. Nature 2016. 4. Bardyn et al. MNRAS 2017. 5. Bentley et al. Nature 2016. 6. Langevin et al. Icarus 2016. 7. Mannel et al. MNRAS 2017. 8. Saïagh PhD Thesis UPE 2014. 9. Lasue et al. Astron. Astrophys. 2007. 10. Nesvorny et al. ApJ 2010. 11. Rowan-Robinson and May MNRAS 2013. 12. Hadamcik et al. PSS 2018.

Published
2018

30. Characterization of the refractory organic matter present in the dust particles of 67P/Churyumov-Gerasimenko

Author

Fray, Nicolas, Baklouti, Donia, Bardyn, Anaïs, Briois, Christelle, Cottin, Hervé, Engrand, Cécile, Fischer, Henning, Hilchenbach, Martin, Isnard, Robin, Le Roy, Léna, Modica, Paola, Paquette, John, Ryno, Jouni, Stenzel, Oliver, Siljeström, Sandra, Thirkell, Laurent, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; The Cometary Secondary Ion Mass Analyser (COSIMA), a miniaturized time-of-flight secondary ion mass spectrometer (ToF-SIMS), is one of the dust particle instruments onboard the orbiter of the Rosetta mission that arrived to comet 67P/Churyumov-Gerasimenko in mid-2014. COSIMA analyses the mineral and organic composition of dust particles that are captured on metal targets exposed to space [1, 2]. The mass spectra acquired by COSIMA show that refractory organic matter is ubiquitous in cometary dust particles [2]. The nature of this carbonaceous material will be discussed. We will highlight the abundance of organic matter in these dust particles as well as the nitrogen to carbon elemental ratio of this refractory organic matter. These results obtained on the dust particles of 67P will be compared to those from other astrophysical objects (carbonaceous chondrites, IDPs, micro-meteorites). This comparison could provide clues on the origin and evolution of the cometary organic matter. References: [1] Hilchenbach, M. et al. (2016) ApJ, 816, L32. [2] Schulz, R. et al. (2015) Nature, 518, 216-218. [3] Fray, N. et al. (2016) Nature, 538, 72-74.

Published
2017

31. Elemental surface composition of comet 67P grains (Rosetta) and of carbonaceous chondrite meteorites - characterized by multivariate mass spectral data (COSIMA)

Author

Varmuza, Kurt, Brandstätter, Franz, Cottin, Hervé, Engrand, Cécile, Ferrière, Ludovic, Filzmoser, Peter, Fray, Nicolas, Hilchenbach, Martin, Hoffmann, Irene, Kissel, Jochen, Koeberl, Christian, Modica, Paola, Paquette, John, Stenzel, Oliver, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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, and 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)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; Dust grains have been collected near the comet 67P/Churyumov-Gerasimenko by the time-of-flight secondary ion mass spectrometer (TOF-SIMS) COSIMA on board of the Rosetta spacecraft. The measured mass spectra contain information about the inorganic and organic composition of the surface of the grains. For a comparison of this cometary material with carbonaceous chondrite meteorites, a twin laboratory instrument of COSIMA has been used to obtain mass spectra from grain surfaces of the meteorites Allende, Lancé, Murchison and Renazzo. Multivariate data analyses, based on signals from selected ions, indicate similarities of the chemical composition of the surfaces of different sample groups, as well as the heterogeneity of the grains. Acknowledgments. Supported by the Austrian Science Fund (FWF), project P 26871-N20. Thanks to the members of the COSIMA team for their contributions.

Published
2017

33. CASTALIA : A mission to a main belt comet

Author

Jones, G. H., Altwegg, K., Bertini, I., Bieler, A., Boehnhardt, H., Bowles, N., Braukhane, A., Capria, M., T., Coates, A. J., Ciarletti, Valérie, Davidsson, B., Engrand, Cécile, Fitzsimmons, A., Gibbings, A., Hainaut, O., Hallmann, M., Herique, Alain, Hilchenbach, M., Homeister, M., Hsieh, H., Jehin, E., Kofman, W., Lara, L. M., Licandro, J., Lowry, S.C., Moreno, F., Muinonen, Karri, Paetzold, M., Penttilä, Antti, Plettmeier, Dirk, Prialnik, D., Marboeuf, U., Marzari, F., Meech, Karen J., Rotundi, A., Smith, A., Snodgrass, C., Thomas, I., Trieloff, M., Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Physikalisches Institut [Bern], Universität Bern [Bern], Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], DLR Institute of Space Systems, German Aerospace Center (DLR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), 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 Physics and Astronomy [Uppsala], Uppsala University, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Department of Mechanical and Aerospace Engineering [Univ Strathclyde], University of Strathclyde [Glasgow], European Southern Observatory (ESO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), OHB Systems AG, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofisica de Canarias (IAC), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Universität zu Köln, Helsinki Institute of Physics (HIP), University of Helsinki, Technische Universität Dresden = Dresden University of Technology (TU Dresden), Tel Aviv University [Tel Aviv], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Universita degli studi di Napoli 'Parthenope' [Napoli], The Open University [Milton Keynes] (OU), Universität Heidelberg [Heidelberg], IMPEC - LATMOS, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Mechanical and Aerospace Engineering [Glasgow], University of Strathclyde, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Technische Universität Dresden (TUD), National Institute for Nuclear Physics (INFN), Cardon, Catherine, Universität Bern [Bern] (UNIBE), Università degli Studi di Padova = University of Padua (Unipd), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), University of Oxford, Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Orbitale Hochtechnologie Bremen (OHB Systems AG), Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Universität zu Köln = University of Cologne, Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Tel Aviv University (TAU), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Universität Heidelberg [Heidelberg] = Heidelberg University, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' ( CISAS ), Universita degli Studi di Padova = University of Padua = Université de Padoue, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), German Aerospace Center ( DLR ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Istituto Nazionale di Astrofisica ( INAF ), 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 ), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysics Research Centre [Belfast] ( ARC ), Queen's University [Belfast] ( QUB ), European Southern Observatory ( ESO ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), University of Hawaii at Manoa ( UHM ), Institute of Astronomy and Astrophysics [Taipei] ( ASIAA ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Instituto de Astrofisica de Canarias ( IAC ), Centre for Astrophysics and Planetary Science [Canterbury] ( CAPS ), University of Helsinki [Helsinki], Helsinki Institute of Physics ( HIP ), Technische Universität Dresden ( TUD ), Istituto Nazionale di Fisica Nucleare, Sezione di Padova ( INFN, Sezione di Padova ), National Institute for Nuclear Physics ( INFN ), and The Open University [Milton Keynes] ( OU )

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

International audience; Main Belt Comets (MBCs), a type of Active Asteroid , constitute a newly identified class of solar system objects. They have stable, asteroid-like orbits and some exhibit a recurrent comet-like appearance. It is believed that they survived the age of the solar system in a dormant state and that their current ice sublimation driven activity only began recently. Buried water ice is the only volatile expected to survive under an insulating surface. Excavation by an impact can expose the ice and trigger the start of MBC activity. We present the case for a mission to one of these objects, to be submitted to the European Space Agency's current call for an M-class mission. The specific science goals of the Castalia mission are: 1. Characterize a new Solar System family, the MBCs, by in-situ investigation 2. Understand the physics of activity on MBCs 3. Directly sample water in the asteroid belt and test if MBCs are a viable source for Earth's water 4. Use the observed structure of an MBC as a tracer of planetary system formation and evolution.

Published
2015

34. Mineralogy and oxygen isotope systematics of magnetite grains and a magnetite‐dolomite assemblage in hydrated fine‐grained Antarctic micrometeorites.

Author

Dobrică, Elena, Ogliore, Ryan C., Engrand, Cécile, Nagashima, Kazuhide, and Brearley, Adrian J.

Subjects
OXYGEN isotopes, MAGNETITE, MINERALOGY, GRAIN, FLUID control, HYDRATION, CARBONACEOUS aerosols
Abstract

We report the mineralogy and texture of magnetite grains, a magnetite‐dolomite assemblage, and the adjacent mineral phases in five hydrated fine‐grained Antarctic micrometeorites (H‐FgMMs). Additionally, we measured the oxygen isotopic composition of magnetite grains and a magnetite‐dolomite assemblage in these samples. Our mineralogical study shows that the secondary phases identified in H‐FgMMs have similar textures and chemical compositions to those described previously in other primitive solar system materials, such as carbonaceous chondrites. However, the oxygen isotopic compositions of magnetite in H‐FgMMs span a range of ∆17O values from +1.3‰ to +4.2‰, which is intermediate between magnetites measured in carbonaceous and ordinary chondrites (CCs and OCs). The δ18O values of magnetites in one H‐FgMM have a ~27‰ mass‐dependent spread in a single 100 × 200 μm particle, indicating that there was a localized control of the fluid composition, probably due to a low water‐to‐rock mass ratio. The ∆17O values of magnetite indicate that H‐FgMMs sampled a different aqueous fluid than ordinary and carbonaceous chondrites, implying that the source of H‐FgMMs is probably distinct from the asteroidal source of CCs and OCs. Additionally, we analyzed the oxygen isotopic composition of a magnetite‐dolomite assemblage in one of the H‐FgMMs (sample 03‐36‐46) to investigate the temperature at which these minerals coprecipitated. We have used the oxygen isotope fractionation between the coexisting magnetite and dolomite to infer a precipitation temperature between 160 and 280 °C for this sample. This alteration temperature is ~100–200 °C warmer than that determined from a calcite‐magnetite assemblage from the CR2 chondrite Al Rais, but similar to the estimated temperature of aqueous alteration for unequilibrated OCs, CIs, and CMs. This suggests that the sample 03‐36‐46 could come from a parent body that was large enough to attain temperatures as high as the OCs, CIs, and CMs, which implies an asteroidal origin for this particular H‐FgMM. [ABSTRACT FROM AUTHOR]

Published
2019
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35. First discovery of meteoritic events in deep Antarctic (EPICA-Dome C) ice cores

Author

Narcisi, Biancamaria, Robert Petit, Jean, Engrand, Cécile, Ente per le Nuove Technologie, l'Energia e l'Ambiente (ENEA), Centro Ricerche Casaccia, Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), European Project for Ice Coring in Antarctica (EPICA), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
Antarctica, micrometeorites, [SDU.STU.GL]Sciences of the Universe [physics]/Earth Sciences/Glaciology, ice core
Abstract

International audience; Two distinct dust layers in the EPICA-Dome C ice core (75°06′S, 123°21′E, East Antarctic Plateau) have been shown to relate to individual meteoritic events. Particles forming these layers, investigated by electron microprobe, show peculiar textural, mineralogical and geochemical features and closely resemble extraterrestrial debris in deep-sea sediments and polar caps. Preliminary estimates of cosmic debris input at the studied layers, obtained from Coulter Counter measurements, are 4–5 orders of magnitude greater than the yearly micrometeorite flux in East Antarctic snow and ice. The cosmic events are accurately dated through glaciological models at 434 ± 6 and 481 ± 6 ka, respectively and are located in the core climatic stratigraphy near the “Mid-Brunhes Event”. This is the first report of well-dated cosmic horizons in deep Antarctic ice cores. It significantly improves the extraterrestrial record of Antarctica and opens new correlation perspectives between long climatic records of the South polar region.

Published
2007

36. Carbonaceous micrometeorites from Antarctica (Invited Review)

Author

Engrand, Cécile, Maurette, Michel, University of California [Los Angeles] (UCLA), University of California, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; Over 100 000 large interplanetary dust particles in the 50-500 pm size range have been recovered in clean conditions from-600 tons of Antarctic melt ice water as both unmelted and partially melteddehydrated micrometeorites and cosmic spherules. Flux measurements in both the Greenland and Antarctica ice sheets indicate that the micrometeorites deliver to the Earth's surface-2OOOx more extraterrestrial material than brought by meteorites. Mineralogical and chemical studies of Antarctic micrometeorites indicate that they are only related to the relatively rare CM and CR carbonaceous chondrite groups, being mostly chondritic carbonaceous objects composed of highly unequilibrated assemblages of anhydrous and hydrous minerals. However, there are also marked differences between these two families of solar system objects, including higher C/O ratios and a very marked depletion of chondrules in micrometeorite matter; hence, they are "chondrites-without-chondrules." Thus, the parent meteoroids of micrometeorites represent a dominant and new population of solar system objects, probably formed in the outer solar system and delivered to the inner solar system by the most appropriate vehicles, comets. One of the major purposes of this paper is to discuss applications of micrometeorite studies that have been previously presented to exobiologists but deal with the synthesis of prebiotic molecules on the early Earth, and more recently, with the early history of the solar system.

Published
1998

37. Interstellar and interplanetary solids in the laboratory.

Author

Dartois, Emmanuel, Alata, Ivan, Engrand, Cécile, Brunetto, Rosario, Duprat, Jean, Pino, Thomas, Quirico, Eric, Remusat, Laurent, Bardin, Noémie, Mostefaoui, Smail, Morinaud, Gilles, Crane, Bruno, Szwec, Nicolas, Delauche, Lucie, Jamme, Frédéric, Sandt, Christophe, Dumas, Paul, and Benvenuti, Piero

Abstract

The composition of interstellar matter is driven by environmental parameters and results from extreme interstellar medium physico-chemical conditions. Astrochemists must rely on remote observations to monitor and analyze the interstellar solids composition. They bring additional information from the study of analogues produced in the laboratory, placed in simulated space environments. Planetologists and cosmochemists access and spectroscopically examine collected extraterrestrial material in the laboratory. Diffuse interstellar medium and molecular clouds observations set constraints on the composition of organic solids that can then be compared with collected extraterrestrial materials analyses, to shed light on their possible links. [ABSTRACT FROM PUBLISHER]

Published
2015
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44. Cometary Dust

Author

Levasseur-Regourd, Anny-Chantal, Agarwal, Jessica, Cottin, Hervé, Engrand, Cécile, Flynn, George, Fulle, Marco, Gombosi, Tamas, Langevin, Yves, Lasue, Jérémie, Mannel, Thurid, Merouane, Sihane, Poch, Olivier, Thomas, Nicolas, and Westphal, Andrew

Subjects
13. Climate action, 520 Astronomy, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, complex mixtures, Astrophysics::Galaxy Astrophysics, respiratory tract diseases
Abstract

This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth’s orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the Sun and from the nucleus. The diverse approaches available to study dust in comets, together with the related theoretical and experimental studies, provide evidence of the composition and physical properties of dust particles, e.g., the presence of a large fraction of carbon in macromolecules, and of aggregates on a wide range of scales. The results have opened vivid discussions on the variety of dust-release processes and on the diversity of dust properties in comets, as well as on the formation of cometary dust, and on its presence in the near-Earth interplanetary medium. These discussions stress the significance of future explorations as a way to decipher the formation and evolution of our Solar System.

45. COSIMA-Rosetta calibration for in situ characterization of 67P/Churyumov–Gerasimenko cometary inorganic compounds.

Author

Krüger, Harald, Stephan, Thomas, Engrand, Cécile, Briois, Christelle, Siljeström, Sandra, Merouane, Sihane, Baklouti, Donia, Fischer, Henning, Fray, Nicolas, Hornung, Klaus, Lehto, Harry, Orthous-Daunay, Francois-Régis, Rynö, Jouni, Schulz, Rita, Silén, Johan, Thirkell, Laurent, Trieloff, Mario, and Hilchenbach, Martin

Subjects
*SECONDARY ion mass spectrometry, *INORGANIC compounds, *INTERPLANETARY dust, *CHURYUMOV-Gerasimenko comet
Abstract

COmetary Secondary Ion Mass Analyzer (COSIMA) is a time-of-flight secondary ion mass spectrometry (TOF-SIMS) instrument on board the Rosetta space mission. COSIMA has been designed to measure the composition of cometary dust particles. It has a mass resolution m /Δ m of 1400 at mass 100 u, thus enabling the discrimination of inorganic mass peaks from organic ones in the mass spectra. We have evaluated the identification capabilities of the reference model of COSIMA for inorganic compounds using a suite of terrestrial minerals that are relevant for cometary science. Ground calibration demonstrated that the performances of the flight model were similar to that of the reference model. The list of minerals used in this study was chosen based on the mineralogy of meteorites, interplanetary dust particles and Stardust samples. It contains anhydrous and hydrous ferromagnesian silicates, refractory silicates and oxides (present in meteoritic Ca–Al-rich inclusions), carbonates, and Fe–Ni sulfides. From the analyses of these minerals, we have calculated relative sensitivity factors for a suite of major and minor elements in order to provide a basis for element quantification for the possible identification of major mineral classes present in the cometary particles. [ABSTRACT FROM AUTHOR]

Published
2015
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46. Orbitrap mass analyser for in situ characterisation of planetary environments: Performance evaluation of a laboratory prototype.

Author

Briois, Christelle, Thissen, Roland, Thirkell, Laurent, Aradj, Kenzi, Bouabdellah, Abdel, Boukrara, Amirouche, Carrasco, Nathalie, Chalumeau, Gilles, Chapelon, Olivier, Colin, Fabrice, Coll, Patrice, Cottin, Hervé, Engrand, Cécile, Grand, Noel, Lebreton, Jean-Pierre, Orthous-Daunay, François-Régis, Pennanech, Cyril, Szopa, Cyril, Vuitton, Véronique, and Zapf, Pascal

Subjects
*PROTOTYPES, *GEOCHEMISTRY, *MASS spectrometry, *NUCLEAR spectroscopy, *INTERPLANETARY dust
Abstract

For decades of space exploration, mass spectrometry has proven to be a reliable instrumentation for the characterisation of the nature and energy of ionic and neutral, atomic and molecular species in the interplanetary medium and upper planetary atmospheres. It has been used as well to analyse the chemical composition of planetary and small bodies environments. The chemical complexity of these environments calls for the need to develop a new generation of mass spectrometers with significantly increased mass resolving power. The recently developed Orbitrap TM mass analyser at ultra-high resolution shows promising adaptability to space instrumentation, offering improved performances for in situ measurements. In this article, we report on our project named “Cosmorbitrap” aiming at demonstrating the adaptability of the Orbitrap technology for in situ space exploration. We present the prototype that was developed in the laboratory for demonstration of both technical feasibility and analytical capabilities. A set of samples containing elements with masses ranging from 9 to 208 u has been used to evaluate the performance of the analyser, in terms of mass resolving power (reaching 474,000 at m / z 9) and ability to discriminate between isobaric interferences, accuracy of mass measurement (below 15 ppm) and determination of relative isotopic abundances (below 5%) of various samples. We observe a good agreement between the results obtained with the prototype and those of a commercial instrument. As the background pressure is a key parameter for in situ exploration of atmosphere planetary bodies, we study the effect of background gas on the performance s of the Cosmorbitrap prototype, showing an upper limit for N 2 in our set-up at 10 −8 mbar. The results demonstrate the strong potential to adapt this technology to space exploration. [ABSTRACT FROM AUTHOR]

Published
2016
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47. Origin of insoluble organic matter in type 1 and 2 chondrites: New clues, new questions.

Author

Quirico, Eric, Orthous-Daunay, François-Régis, Beck, Pierre, Bonal, Lydie, Brunetto, Rosario, Dartois, Emmanuel, Pino, Thomas, Montagnac, Gilles, Rouzaud, Jean-Noël, Engrand, Cécile, and Duprat, Jean

Subjects
*ORGANIC compounds, *AROMATIC compounds, *CARBONACEOUS chondrites (Meteorites), *METAMORPHISM (Geology), *CROSSLINKING (Polymerization), *AQUEOUS solutions
Abstract

Abstract: Insoluble organic matter (IOM) extracted from primitive chondrites is a polyaromatic solid with a structure and composition resembling that of terrestrial kerogens. A survey of its composition and structure has been carried out on a series of 27 CR, CM, CI and ungrouped C2 carbonaceous chondrites (Tagish Lake, Bells, Essebi, Acfer 094) using infrared and multi-wavelength Raman micro-spectroscopy (244, 514 and 785nm laser excitations). The results show that chondritic IOM from PCA 91008 (CM2), WIS 91600 (CM2), QUE 93005 (CM2), Tagish Lake (C2 ungrouped) and possibly Cold Bokkeveld (CM2) has been subjected to the past action of short duration thermal metamorphism, presumably triggered by impacts. The IOM in most of the CM chondrites that experienced moderate to heavy aqueous alteration may have been slightly modified by collision-induced heating. However, even IOM from chondrites that escaped significant thermal metamorphism displays Raman characteristics consistent with a formation by thermal processing, either in the protosolar disk or in the parent body. An alternative energetic process to thermal heating is ion irradiation. After thoroughly analyzing both these scenarii, no conclusion can be drawn as to which is the most plausible mechanism nor whether the heating process took place prior or after accretion. The results show for the first time that the width of the G band in spectra collected with a 514nm excitation correlates with the O/C atomic ratio, suggesting a major role of oxygen in the cross-linking of polyaromatic units. [Copyright &y& Elsevier]

Published
2014
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48. A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk.

Author

Berné O, Habart E, Peeters E, Schroetter I, Canin A, Sidhu A, Chown R, Bron E, Haworth TJ, Klaassen P, Trahin B, Van De Putte D, Alarcón F, Zannese M, Abergel A, Bergin EA, Bernard-Salas J, Boersma C, Cami J, Cuadrado S, Dartois E, Dicken D, Elyajouri M, Fuente A, Goicoechea JR, Gordon KD, Issa L, Joblin C, Kannavou O, Khan B, Lacinbala O, Languignon D, Le Gal R, Maragkoudakis A, Meshaka R, Okada Y, Onaka T, Pasquini S, Pound MW, Robberto M, Röllig M, Schefter B, Schirmer T, Simmer T, Tabone B, Tielens AGGM, Vicente S, Wolfire MG, Aleman I, Allamandola L, Auchettl R, Baratta GA, Baruteau C, Bejaoui S, Bera PP, Black JH, Boulanger F, Bouwman J, Brandl B, Brechignac P, Brünken S, Buragohain M, Burkhardt A, Candian A, Cazaux S, Cernicharo J, Chabot M, Chakraborty S, Champion J, Colgan SWJ, Cooke IR, Coutens A, Cox NLJ, Demyk K, Meyer JD, Engrand C, Foschino S, García-Lario P, Gavilan L, Gerin M, Godard M, Gottlieb CA, Guillard P, Gusdorf A, Hartigan P, He J, Herbst E, Hornekaer L, Jäger C, Janot-Pacheco E, Kaufman M, Kemper F, Kendrew S, Kirsanova MS, Knight C, Kwok S, Labiano Á, Lai TS, Lee TJ, Lefloch B, Le Petit F, Li A, Linz H, Mackie CJ, Madden SC, Mascetti J, McGuire BA, Merino P, Micelotta ER, Morse JA, Mulas G, Neelamkodan N, Ohsawa R, Paladini R, Palumbo ME, Pathak A, Pendleton YJ, Petrignani A, Pino T, Puga E, Rangwala N, Rapacioli M, Ricca A, Roman-Duval J, Roueff E, Rouillé G, Salama F, Sales DA, Sandstrom K, Sarre P, Sciamma-O'Brien E, Sellgren K, Shannon MJ, Simonnin A, Shenoy SS, Teyssier D, Thomas RD, Togi A, Verstraete L, Witt AN, Wootten A, Ysard N, Zettergren H, Zhang Y, Zhang ZE, and Zhen J

Abstract

Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photodissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, which affects planet formation within the disks. We report James Webb Space Telescope and Atacama Large Millimeter Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modeling their kinematics and excitation allowed us to constrain the physical conditions within the gas. We quantified the mass-loss rate induced by the FUV irradiation and found that it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk.

Published
2024
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49. Macromolecular organic matter in samples of the asteroid (162173) Ryugu.

Author

Yabuta H, Cody GD, Engrand C, Kebukawa Y, De Gregorio B, Bonal L, Remusat L, Stroud R, Quirico E, Nittler L, Hashiguchi M, Komatsu M, Okumura T, Mathurin J, Dartois E, Duprat J, Takahashi Y, Takeichi Y, Kilcoyne D, Yamashita S, Dazzi A, Deniset-Besseau A, Sandford S, Martins Z, Tamenori Y, Ohigashi T, Suga H, Wakabayashi D, Verdier-Paoletti M, Mostefaoui S, Montagnac G, Barosch J, Kamide K, Shigenaka M, Bejach L, Matsumoto M, Enokido Y, Noguchi T, Yurimoto H, Nakamura T, Okazaki R, Naraoka H, Sakamoto K, Connolly HC Jr, Lauretta DS, Abe M, Okada T, Yada T, Nishimura M, Yogata K, Nakato A, Yoshitake M, Iwamae A, Furuya S, Hatakeda K, Miyazaki A, Soejima H, Hitomi Y, Kumagai K, Usui T, Hayashi T, Yamamoto D, Fukai R, Sugita S, Kitazato K, Hirata N, Honda R, Morota T, Tatsumi E, Sakatani N, Namiki N, Matsumoto K, Noguchi R, Wada K, Senshu H, Ogawa K, Yokota Y, Ishihara Y, Shimaki Y, Yamada M, Honda C, Michikami T, Matsuoka M, Hirata N, Arakawa M, Okamoto C, Ishiguro M, Jaumann R, Bibring JP, Grott M, Schröder S, Otto K, Pilorget C, Schmitz N, Biele J, Ho TM, Moussi-Soffys A, Miura A, Noda H, Yamada T, Yoshihara K, Kawahara K, Ikeda H, Yamamoto Y, Shirai K, Kikuchi S, Ogawa N, Takeuchi H, Ono G, Mimasu Y, Yoshikawa K, Takei Y, Fujii A, Iijima YI, Nakazawa S, Hosoda S, Iwata T, Hayakawa M, Sawada H, Yano H, Tsukizaki R, Ozaki M, Terui F, Tanaka S, Fujimoto M, Yoshikawa M, Saiki T, Tachibana S, Watanabe SI, and Tsuda Y

Abstract

Samples of the carbonaceous asteroid (162173) Ryugu were collected and brought to Earth by the Hayabusa2 spacecraft. We investigated the macromolecular organic matter in Ryugu samples and found that it contains aromatic and aliphatic carbon, ketone, and carboxyl functional groups. The spectroscopic features of the organic matter are consistent with those in chemically primitive carbonaceous chondrite meteorites that experienced parent-body aqueous alteration (reactions with liquid water). The morphology of the organic carbon includes nanoglobules and diffuse carbon associated with phyllosilicate and carbonate minerals. Deuterium and/or nitrogen-15 enrichments indicate that the organic matter formed in a cold molecular cloud or the presolar nebula. The diversity of the organic matter indicates variable levels of aqueous alteration on Ryugu's parent body.

Published
2023
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