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51. Distribution of phyllosilicates on the surface of Ceres

Author

Ernesto Palomba, Carol A. Polanskey, Maria Teresa Capria, Filippo Giacomo Carrozzo, Gianfranco Magni, Julie Castillo-Rogez, Eleonora Ammannito, Sergio Fonte, Alessandro Frigeri, T. B. McCord, Bethany L. Ehlmann, Andrea Longobardo, Steve Joy, Christopher T. Russell, Francesca Zambon, M.C. Desanctis, Mauro Ciarniello, Ralf Jaumann, Harry Y. McSween, Andrea Raponi, J. Ph. Combe, Carol A. Raymond, Michael J. Toplis, Lucy A. McFadden, Paul M. Schenk, C. M. Pieters, Marco Giardino, Simone Marchi, Federico Tosi, Marc D. Rayman, and Fabrizio Capaccioni

Subjects
Surface (mathematics), Multidisciplinary, 010504 meteorology & atmospheric sciences, Spectrometer, Dwarf planet, Mineralogy, Spatial distribution, DAWN, Phyllosilicates, 01 natural sciences, Astrobiology, Meteorite, Asteroid, 0103 physical sciences, Ceres, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Relative species abundance, Geology, 0105 earth and related environmental sciences
Abstract

INTRODUCTIONThe surface of the dwarf planet Ceres is known to host phyllosilicate minerals, but their distribution and origin have not previously been determined. Phyllosilicates are hydrated silicates, and their presence on the surface of Ceres is intriguing given that their structure evolves through an aqueous alteration process. In addition, some phyllosilicates are known to bear NH4, which places a constraint on the pH and redox conditions during the evolution of Ceres. We studied the distribution of phyllosilicates across the planet’s surface to better understand the evolutionary pathway of Ceres.RATIONALEUsing the data acquired by the mapping spectrometer (VIR) onboard the Dawn spacecraft, we mapped the spatial distribution of different minerals on Ceres on the basis of their diagnostic absorption features in visible and infrared spectra. We studied the phyllosilicates through their OH-stretch fundamental absorption at about 2.7 µm and through the NH4absorption at about 3.1 µm. From our composition maps, we infer the origin of the materials identified.RESULTSWe found that Mg- and NH4-bearing phyllosilicates are ubiquitous across the surface of Ceres and that their chemical composition is fairly uniform. The widespread presence of these two types of minerals is a strong indication of a global and extensive aqueous alteration—i.e., the presence of water at some point in Ceres’ geological history. Although the detected phyllosilicates are compositionally homogeneous, we found variations in the intensity of their absorption features in the 3-µm region of the reflectance spectrum. Such variations are likely due to spatial variability in relative mineral abundance (see the figure).CONCLUSIONThe large-scale regional variations evident in the figure suggest lateral heterogeneity in surficial phyllosilicate abundance on scales of several hundreds of kilometers. Terrains associated with the Kerwan crater (higher concentration of phyllosilicates) appear smooth, whereas the Yalode crater (lower concentration of phyllosilicates) is characterized by both smooth and rugged terrains. These distinct morphologies and phyllosilicate concentrations observed in two craters that are similar in size may reflect different compositions and/or rheological properties. On top of this large-scale lateral heterogeneity, small-scale variations associated with individual craters could result from different proportions of mixed materials in a stratified upper crustal layer that has been exposed by impacts. Variations associated with fresh craters, such as the 34-km-diameter Haulani, indicate the presence of crustal variations over a vertical scale of a few kilometers, whereas much larger craters, such as the 126-km-diameter Dantu, suggest that such stratification may extend for at least several tens of kilometers.Abundance maps.Qualitative maps of the abundances of (top) phyllosilicates and (bottom) NH4, based on the depth of their absorption features. The two maps have a similar global pattern, although they differ in some localized regions such as Urvara. The scale bar is valid at the equator.

Published
2016

52. Exposed water ice on the nucleus of comet 67P/Churyumov-Gerasimenko

Author

Giancarlo Bellucci, Katrin Stephan, Yves Langevin, Sergio Fonti, G. Peter, Gianrico Filacchione, Ulrich Schade, G. P. Tozzi, Jacques Crovisier, Costanzo Federico, Eleonora Ammannito, M. I. Blecka, S. Jacquinod, Jean-Michel Reess, M. Cartacci, Michael R. Combi, Vito Mennella, Federico Tosi, Marcello Fulchignoni, Armando Blanco, Giuseppe Piccioni, Roberto Orosei, Bernard Schmitt, Andrea Longobardo, Giovanna Rinaldi, Ralf Jaumann, Vincenzo Orofino, Alessandra Migliorini, Andrea Raponi, Pierre Drossart, M. Combes, David Kappel, Mauro Ciarniello, D. Despan, Murthy S. Gudipati, C. Leyrat, T. Encrenaz, Ernesto Palomba, Andrea Cicchetti, Fabrizio Capaccioni, Michelangelo Formisano, Maria Teresa Capria, Romolo Politi, Dominique Bockelée-Morvan, Stefano Mottola, Enrico Flamini, Pierre Beck, L. Moroz, Gianfranco Magni, U. Fink, Eric Quirico, Fredric W. Taylor, Sonia Fornasier, J-Ph. Combe, F. Merlin, Jean-Pierre Bibring, N. Biver, M. C. De Sanctis, Florence Henry, Uri Carsenty, M. A. Barucci, Gabriele Arnold, Y. Hello, Patrick G. J. Irwin, R. W. Carlson, Wing-Huen Ip, E. Kuehrt, Kathrin Markus, Davide Grassi, S. Giuppi, Raffaella Noschese, Alessandro Frigeri, F. Mancarella, Stéphane Erard, Luigi Colangeli, Lydie Bonal, T. B. McCord, J. Benkhoff, D. Tiphene, Priscilla Cerroni, G., Filacchione, M. C., De Sancti, F., Capaccioni, A., Raponi, F., Tosi, M., Ciarniello, P., Cerroni, G., Piccioni, M. T., Capria, E., Palomba, G., Bellucci, S., Erard, D., Bockelee Morvan, C., Leyrat, G., Arnold, M. A., Barucci, M., Fulchignoni, B., Schmitt, E., Quirico, R., Jaumann, K., Stephan, A., Longobardo, V., Mennella, A., Migliorini, E., Ammannito, J., Benkhoff, J. P., Bibring, Blanco, Armando, M. I., Blecka, R., Carlson, U., Carsenty, L., Colangeli, M., Combe, M., Combi, J., Crovisier, P., Drossart, T., Encrenaz, C., Federico, U., Fink, Fonti, Sergio, W. H., Ip, P., Irwin, E., Kuehrt, Y., Langevin, G., Magni, T., Mccord, L., Moroz, S., Mottola, Orofino, Vincenzo, U., Schade, F., Taylor, D., Tiphene, G. P., Tozzi, P., Beck, N., Biver, L., Bonal, Combe, J. P. h., D., Despan, E., Flamini, M., Formisano, S., Fornasier, A., Frigeri, D., Grassi, M. S., Gudipati, D., Kappel, Mancarella, Francesca, K., Marku, F., Merlin, R., Orosei, G., Rinaldi, M., Cartacci, A., Cicchetti, S., Giuppi, Y., Hello, F., Henry, S., Jacquinod, J. M., Ree, R., Noschese, R., Politi, G., Peter, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Mécanique Textiles (LPMT), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-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)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), German Aerospace Center (DLR), Deutsches Zentrum für Luft- und Raumfahrt (DLR), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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)-Centre National d’Études Spatiales [Paris] (CNES), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), INAF - Osservatorio Astronomico di Capodimonte (OAC), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Instituto de Estudos Avançados (IEAV), Institut, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Dipartimento di Fisica, Università degli studi di Lecce, Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Department of Physics [Oxford], University of Oxford, Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], DLR Institute of Planetary Research, Department of Physics [Lecce], Università del Salento [Lecce], INAF - Osservatorio Astrofisico di Arcetri (OAA), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Alenia Aerospazio, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), JDS Uniphase/Cronos, USA, JDS Uniphase/Cronos, CNR-IASF, Istituti di Ricovero e Cura a Carattere Scientifico (IRCCS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d’Océanologie et de Géosciences (LOG) - UMR 8187 (LOG), Institut national des sciences de l'Univers (INSU - CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Nord]), Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-ENSITM-Matériaux et nanosciences d'Alsace, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Polska Akademia Nauk (PAN), University of Oxford [Oxford], Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Centre National de la Recherche Scientifique (CNRS), Université de Lille-Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique (CNRS), ENSITM-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
Materials science, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Comet, Mineralogy, comet 67P, 01 natural sciences, water ice, Astrobiology, Diffusion, 0103 physical sciences, Rosetta, medicine, Diffusion (business), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Multidisciplinary, Meteoroid, Spectrum Analysis, Ice, food and beverages, Meteoroids, VIRTIS, Debris, Asteroids, Grain growth, medicine.anatomical_structure, 13. Climate action, comets and Kuiper belt Early solar system, Gases, Layering, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Nucleus, Water vapor
Abstract

Although water vapour is the main species observed in the coma of comet 67P/Churyumov–Gerasimenko1, 2 and water is the major constituent of cometary nuclei3, 4, limited evidence for exposed water-ice regions on the surface of the nucleus has been found so far5, 6. The absence of large regions of exposed water ice seems a common finding on the surfaces of many of the comets observed so far7, 8, 9. The nucleus of 67P/Churyumov–Gerasimenko appears to be fairly uniformly coated with dark, dehydrated, refractory and organic-rich material10. Here we report the identification at infrared wavelengths of water ice on two debris falls in the Imhotep region of the nucleus. The ice has been exposed on the walls of elevated structures and at the base of the walls. A quantitative derivation of the abundance of ice in these regions indicates the presence of millimetre-sized pure water-ice grains, considerably larger than in all previous observations6, 7, 8, 9. Although micrometre-sized water-ice grains are the usual result of vapour recondensation in ice-free layers6, the occurrence of millimetre-sized grains of pure ice as observed in the Imhotep debris falls is best explained by grain growth by vapour diffusion in ice-rich layers, or by sintering. As a consequence of these processes, the nucleus can develop an extended and complex coating in which the outer dehydrated crust10 is superimposed on layers enriched in water ice. The stratigraphy observed on 67P/Churyumov–Gerasimenko11, 12 is therefore the result of evolutionary processes affecting the uppermost metres of the nucleus and does not necessarily require a global layering to have occurred at the time of the comet’s formation.

Published
2016
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53. Mineralogical mapping of the Occator Quadrangle

Author

Federico Tosi, Alessandro Frigeri, Debra Buczkowski, Andrea Longobardo, Maria Teresa Capria, Ernesto Palomba, Francesca Zambon, Andrea Raponi, Marco Giardino, Maria Cristina De Sanctis, Sergio Fonte, Filippo Giacomo Carrozzo, Carol A. Raymond, Eleonora Ammannito, Mauro Ciarniello, Christopher T. Russell, Katrin Stephan, A. Galiano, and Lucy A. McFadden

Subjects
Planetengeologie, Quadrangle, Occator, Geochemistry, Ceres, Mineralogy, Geology, Dawn
Published
2016

54. Exploring the asteroid belt with ion propulsion: Dawn mission history, status and plans

Author

Thomas H. Prettyman, Lucy A. McFadden, M. C. De Sanctis, M. A. Barucci, Holger Sierks, Harry Y. McSween, Carol A. Raymond, T. B. McCord, Ulrich R. Christensen, G. Neukum, Christopher T. Russell, Carle M. Pieters, William C. Feldman, Andreas Nathues, David E. Smith, Maria T. Zuber, H. U. Keller, Ralf Jaumann, Maria Teresa Capria, Alex S. Konopliv, Faith Vilas, Richard P. Binzel, Tilman Spohn, Stefano Mottola, Kevin D. McKeegan, Angioletta Coradini, Mark V. Sykes, Institute of Geophysics and Planetary Physics, University of California, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Università degli Studi di Roma Tor Vergata [Roma], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, DLR - German Aerospace Center, Jet Propulsion Laboratory, California Institute of Technology (JPL), Space Science Institute, Winthrop, Department of Astronomy, University of Maryland, Department of Earth and Planetary Science, University of Tennessee, IGGG, Freie Universität Berlin (IGGG), Department of Geological Science, Brown University, LANL, MS D466 NIS-1, Space & Atmospheric Sci., Los Alamos, NASA/Goddard Space Flight Center (NASA/GSFC), and MMT Observatory, University of Arizona

Subjects
Ion propulsion, Atmospheric Science, Solar System, Ion thruster, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Asteroids, Astrobiology, Vesta, Geophysics, Space and Planetary Science, Asteroid, Ceres, General Earth and Planetary Sciences, Asteroid belt, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hygeia, Geology
Abstract

International audience; In this report, we describe the journey Dawn has taken in the recent past, its present status, and its future mission. The overall objective of Dawn is to explore backward in time via its observations of the primitive bodies, Vesta and Ceres. Thus Dawn embarks on three journeys. The first is its tumultuous temporal terrestrial trek during development. The second is its soon-to-be voyage in space to 4 Vesta, the second most massive asteroid in the main belt, and to 1 Ceres, the most massive. The third is its journey backward in time to infer the conditions as the solar system was formed. Finally, we discuss how it is possible to go back even further in time, beyond the horizon of the Dawn mission to obtain "pre Dawn" observations at 10 Hygiea, the fourth most massive asteroid, and one more primitive than Vesta and Ceres.

Published
2007
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55. VIRTIS on Rosetta: a unique technique to observe comet 67P/Churyumov-Gerasimenko – first results and prospects

Author

Priscilla Cerroni, Ernesto Palomba, Gabriele Arnold, David Kappel, Frederico Tosi, Kathrin Markus, Maria Antonietta Barucci, Bernard Schmitt, Fabrizio Capaccioni, Gian Paolo Tozzi, Maria Teresa Capria, Stéphane Erard, Giuseppe Piccioni, Maria Cristina De Sanctis, Alessandra Migliorini, Gianrico Filacchione, Dominique Bockelée-Morvan, C. Leyrat, and Pierre Drossart

Subjects
Physics, spectroscopy, Spectrometer, business.industry, Leitungsbereich PF, Comet, Phase (waves), Imaging spectrometer, Astronomy, Coma (optics), Field of view, Planetary remote sensing, Optics, Rosetta, comets, Spectral resolution, business, Spectroscopy
Abstract

VIRTIS aboard ESA’s Rosetta mission is a complex imaging spectrometer that combines three unique data channels in one compact instrument to study nucleus and coma of comet 67P/Churyumov-Gerasimenko. Two of the spectral channels are dedicated to spectral mapping (-M) at moderate spectral resolution in the range from 0.25 to 5.1 μm. The third channel is devoted to high resolution spectroscopy (-H) between 2 and 5 μm. The VIRTIS-H field of view is approximately centered in the middle of the -M image. The spectral sampling of VIRTIS-M is 1.8 nm/band below 1 μm and 9.7 nm/band between 1-5 μm, while for VIRTIS-H λ/Δλ= 1300-3000 in the 2-5 μm range. This paper describes selected findings during the pre-landing phase of Philae’s robotic subsystem and the comet’s escort phase as well as prospects of further observations. The preliminary results include studies of surface composition, coma analyses, and temperature retrieval for the nucleus surface-coma system demonstrating the capability of the instrument.

Published
2015
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56. Interpretation of thermal emission. I. The effect of roughness for spatially resolved atmosphereless bodies

Author

Pedro J. Gutiérrez, Alessandro Maturilli, Joern Helbert, Magdalena Wilska, Laurent Jorda, Joshua L. Bandfield, Joshua P. Emery, Olivier Groussin, Maria Teresa Capria, Thomas Mueller, Björn Davidsson, Hans Rickman, Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], DLR Institute of Planetary Research, German Aerospace Center (DLR), and 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)

Subjects
Surface (mathematics), Solar System, Materials science, 010504 meteorology & atmospheric sciences, Surface finish, surfaces, 01 natural sciences, Optics, Fractal, 0103 physical sciences, Surface roughness, Comets, surface, Moon, 010303 astronomy & astrophysics, Spectroscopy, 0105 earth and related environmental sciences, Spacecraft, Infrared observations, business.industry, nucleus, Astronomy and Astrophysics, Mechanics, Spherical segment, Asteroids, Wavelength, Space and Planetary Science, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Spacecraft observations of atmosphereless Solar System bodies, combined with thermophysical modeling, provide important information about the thermal inertia and degree of surface roughness of these bodies. The thermophysical models rely on various methods of generating topography, the most common being the concave spherical segment. We here compare the properties of thermal emission for a number of different topographies - concave spherical segments, random Gaussians, fractals and parallel sinusoidal trenches - for various illumination and viewing geometries, degrees of surface roughness and wavelengths. We find that the thermal emission is strongly dependent on roughness type, even when the degrees of roughness are identical, for certain illumination and viewing geometries. The systematic usage of any single topography model may therefore bias determinations of thermal inertia and level of roughness. We outline strategies that may be employed during spacecraft observations to disentangle thermal inertia, level of roughness and type of topography. We also compare the numerically complex and time consuming full-scale thermophysical models with a simplified statistical approach, which is fairly easy to implement and quick to run. We conclude that the simplified statistical approach is similar to thermophysical models for cases tested here, which enables the user to analyze huge amounts of spectral data at a low numerical cost. (C) 2015 Elsevier Inc. All rights reserved.

Published
2015
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57. Catalog of the emission lines in the visible spectrum of comet 153P/Ikeya-Zhang

Author

Maria Teresa Capria, M. C. De Sanctis, and Gabriele Cremonese

Subjects
Physics, Space and Planetary Science, Comet, Visible range, Astronomy, High resolution, Astronomy and Astrophysics, Emission spectrum, Astrophysics, Spectroscopy, Spectrograph, Visible spectrum
Abstract

A program of high resolution spectroscopy of comets is being conducted at TNG (Canary Islands) using the echelle spectrograph SARG. The aim of the program is to catalogue emission lines in the visible range of various comets, compare them and possibly identify the many existing unknown lines. As a first step, we catalogued the lines in the spectrum of the comet 153P/Ikeya-Zhang and compared them with the lines already listed in existing catalogues. The comet was observed with SARG on the night 19–20 of April, 2002, with a short slit covering the spectral range of 4620–7920 A and with a resolving power $R=57\,000$, finding 8468 emission lines.

Published
2006
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58. V-type asteroids: A mineralogical study

Author

Maria Teresa Capria, Maria Cristina De Sanctis, Daniela Lazzaro, Javier Licandro, and Rene Duffard

Subjects
Basalt, Atmospheric Science, Geophysics, Meteorite, Space and Planetary Science, Asteroid, Aerospace Engineering, General Earth and Planetary Sciences, Parameter distribution, Astronomy and Astrophysics, Achondrite, Geology, Astrobiology
Abstract

The relation among V-type asteroids in the Main Belt, the large basaltic asteroid (4) Vesta and the HED meteorites is a long standing issue. To better constraint this relation we analysed the spectral parameter distribution of a sample of V-type asteroids, located in the vicinity of (4) Vesta, and of basaltic achondrites meteorites. Our results indicate that among the V-type asteroids there exist slightly distinct mineralogies which could be explained either as coming from different depths of the asteroid (4) Vesta or from different bodies.

Published
2006
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59. 67P/Churyumov–Gerasimenko nucleus model: Portrayal of the Rosetta target

Author

M. C. De Sanctis, Maria Teresa Capria, and Angioletta Coradini

Subjects
Physics, Atmospheric Science, Comet, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Close encounter, Astrophysics, Thermal conduction, Geophysics, medicine.anatomical_structure, Space and Planetary Science, Comet nucleus, Thermal, Moment (physics), medicine, General Earth and Planetary Sciences, Event (particle physics), Nucleus
Abstract

Rosetta is a cornerstone ESA mission dedicated to the detailed study of a comet nucleus before and after the onset of activity. Comet 67P/Churyumov–Gerasimenko is the new Rosetta target. At the moment, little is known about this comet, but the successful design of the ROSETTA mission requires some preliminary knowledge of the comet’s physical parameters. In fact, surface and interior temperature, day–night variations, onset of activity, percentage of active surface, intensity of different gas and dust fluxes are needed to select safe orbits around the comet and to optimize the scientific return. These quantities cannot be determined only through ground-based observations, so predictive models of the thermal evolution and differentiation of a cometary nucleus are necessary. We have developed a comet nucleus thermal evolution model that helps in the estimations of the above quantities. The ideal nucleus is an initially homogeneous and porous sphere, composed by a mixture of different ices and dust particles. The results have been computed with a numerical code solving simultaneously the heat conduction and gas diffusion equations through an idealized spherical comet nucleus. We show the results obtained applying this model to a comet nucleus with the characteristics of Churyumov–Gerasimenko. The results indicate that the peculiar dynamical history has a strong effect on the comet with the formation of a dust mantle before the 1959 close encounter. After that event, the perihelion distance was reduced and the comet was probably “reactivated”. In our model, we see a slight increase of the activity passage after passage. We found a good agreement between the model results and the few data available.

Published
2006
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60. Thermal evolution model of 67P/Churyumov-Gerasimenko, the new Rosetta target

Author

Angioletta Coradini, Maria Teresa Capria, and M. C. De Sanctis

Subjects
Physics, Diffusion equation, Comet, Astronomy, Astronomy and Astrophysics, Astrophysics, Thermal conduction, medicine.anatomical_structure, Space and Planetary Science, Comet nucleus, Physics::Space Physics, Thermal, Moment (physics), Orbit (dynamics), medicine, Astrophysics::Earth and Planetary Astrophysics, Nucleus
Abstract

Rosetta, the ESA mission dedicated to the detailed study of a comet nucleus before and alter the onset of activity, will arrive at Comet 67P/Churyurnov-Gerasimenko in 2014. At the moment, little is known about this comet. but the successful design of the ROSETTA mission requires some preliminary knowledge of'the comet physical parameters. These quantities cannot be determined only through ground-based observations, so predictive models of the thermal evolution and differentiation of the cometary nucleus are necessary. We have developed a comet nucleus thermal evolution model that helps in the estimation of the above quantities. The results have been computed with a numerical code solving simultaneously the heat conduction and gas diffusion equations through an idealized spherical comet nucleus and we show the results obtained applying this model to a comet nucleus with the characteristics of Churyumov-Gerasimcnko. Our models indicate that the peculiar dynamical history has a strong effect on the comet: during the orbital stage at large heliocentric distance the comet was covered by a dust crust that is removed when the comet arrives at the present orbit. The computed gas fluxes are in general agreement with those estimated from the observations.

Published
2005
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61. O($^{\mathsf 1}$S) and O($^{\mathsf 1}$D) emission lines in the spectrum of 153P/2002 C1 (Ikeya-Zhang)

Author

M. C. De Sanctis, Gabriele Cremonese, Maria Teresa Capria, and Anil Bhardwaj

Subjects
Physics, Space and Planetary Science, Green line, Comet, High resolution, Astronomy and Astrophysics, Emission spectrum, Astrophysics, Spectroscopy, Intensity ratio, Spectrograph
Abstract

High resolution spectroscopy observation of comet 153P/2002 C1 Ikeya-Zhang was performed on April 20, 2002 with the echelle spectrograph SARG on the 3.5 m Telescopio Nazionale Galileo in La Palma. The atomic O emission lines at 5577, 6360 and 6363 A are clearly visible in the spectrum. We determined the intensity ratio of the green line to the sum of the red lines. In order to verify the hypothesis that water is the main parent species of these emissions, the result was compared with the value obtained from a coupled chemistry-transport model. The measured value for the green to red ratio, 0.12 ± 0.1, agrees quite well with the value obtained from the model. This led us to conclude that during the observation water was the parent species of atomic O lines.

Published
2005
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62. The interior of outer Solar System bodies

Author

Maria Teresa Capria and Angioletta Coradini

Subjects
Physics, Solar System, Planetesimal, Jumping-Jupiter scenario, Space and Planetary Science, Nice model, Astronomy, Astronomy and Astrophysics, Formation and evolution of the Solar System, Astrobiology
Published
2005
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63. Mineralogical characterization of some basaltic asteroids in the neighborhood of (4) Vesta: first results

Author

Daniela Lazzaro, Javier Licandro, Rene Duffard, Jorge Márcio Carvano, Maria Teresa Capria, and Maria Cristina De Sanctis

Subjects
Basalt, Solar System, Space and Planetary Science, Asteroid, Astronomy and Astrophysics, Pyroxene, Reflectivity, Geology, Astrobiology, Characterization (materials science)
Abstract

We present reflectance spectra of 19 V-type asteroids obtained at the 3.6 m Telescopio Nazionale Galileo covering 0.8 to 2.5 μm. For 8 of these asteroids we obtained also visible spectra in the same observational run. The range from 0.8 to 2.5 μm, encompassing the 1 and 2 μm pyroxene features, allows a precise mineralogical characterization of these asteroids. The obtained data suggests the possible coexistence of distinct mineralogical groups among the V-type asteroids, either probing different layers of (4) Vesta or coming from different bodies. No clear correlation was found between mineralogies and the objects being, or not, member of the Vesta dynamical family.

Published
2004
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64. Spin Temperatures of Ammonia and Water Molecules in Comets

Author

Maria Teresa Capria, Jun-ichi Watanabe, Hideyo Kawakita, Maria Cristina De Sanctis, Tetsuharu Fuse, Reiko Furusho, and Gabriele Cremonese

Subjects
Physics, Ammonia, chemistry.chemical_compound, chemistry, Space and Planetary Science, Abundance (chemistry), Chemical physics, Error bar, Comet, Molecule, Astronomy and Astrophysics, Astrophysics, Spin (physics)
Abstract

The nuclear spin temperature, which is derived from the ortho-to-para abundance ratio of molecules measured in cometary comae, is a clue to the formation conditions of cometary materials, especially the physical temperature at which the molecules were formed. In this paper we present new results for the nuclear spin temperatures of ammonia in comets Hale-Bopp (C/1995 O1) and 153P/Ikeya-Zhang based on observations of NH2 at 26 and 32 K, respectively. These results are similar to previous measurements in two other comets, and the nuclear spin temperatures of ammonia in the four comets are concentrated at about 30 K. We emphasize that the nuclear spin temperatures of water measured thus far have also been about 30 K. In particular, the spin temperatures of ammonia and water are equal to each other within ±1 σ error bars in the case of comet Hale-Bopp. These nuclear spin temperatures of ammonia and water were measured under quite different conditions (heliocentric distances and gas production rates). There is no clear trend between the nuclear spin temperatures and the heliocentric distances, the gas production rates, or the orbital periods of the comets. The possibilities of the ortho-to-para conversion in the coma and in the nucleus are discussed. The present data set implies that the ortho-to-para ratios were not altered after the molecules were incorporated into the cometary nuclei. It appears that cometary ammonia and water molecules formed on cold grains at about 30 K.

Published
2004
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65. Numerical simulations of the radiance from the comet 46P/Wirtanen in the various configurations of the measurements during 'Rosetta' mission

Author

Maria Teresa Capria, Angioletta Coradini, M. C. De Sanctis, and M. I. Blecka

Subjects
Physics, Atmospheric Science, Spectrometer, Comet, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Coma (optics), Radiation, Spectral line, law.invention, Orbiter, Geophysics, Space and Planetary Science, law, Radiance, General Earth and Planetary Sciences, Zenith
Abstract

The work we present deals with the spectrometric measurements of VIRTIS instrument of the Comet P/Wirtanen planned for the Rosetta mission. This spectrometer can monitor (VIRTIS M channel: 0.250μm – 0.980μm; Δκ=20cm −1 ; 0.980 – 5.0 μm; Δκ = 5cm −1 ; VIRTIS H channel: 2.0 μm – 5.0 μm; Δκ=2cm −1 ) the nucleus and the coma in order to provide a general picture of coma's composition, the production of gas and dust, the relationship of coma production to surface composition and the structure and variation of mineralogy of the nucleus surface. During the mission the observation conditions of the spectroscopic investigation change due to different relative positions spacecraft/comet, and to the different illumination conditions of the surface at various distances of the comet to the Sun. The nucleus surface is continuously modified by the ice sublimation accompanied by gas and dust emission. Consequently the surface also its spectrophotometric properties changes and their monitoring can give a new insight. The important role of simulations is to predict the results of measurements in various experimental condition what, in the future, can help in interpretation of the measured data. In this paper the first results of our simulation the radiance from the comet in the 0.25–5.0μm spectral range at two distances from the Sun (∼1AU and ∼3AU) are shown. The distance between the Rosetta orbiter and the nucleus surface as well as the sun zenith angles are taken into account according to the Rosetta mission phases. In fact the surface and coma properties vary along the comet orbit, and should be taken into account in our calculations. The optical parameters of the dust on the surface (e.g. reflectance) and in the coma (e.g. Q ext ) were calculated from optical constants of possible comet analogues. The thermodynamic parameters of the comet are taken from the models of comet evolution. Through this kind of modelling it is possible to identify the surface characteristics in spectra of the radiation from the surface of nucleus transmitted through the coma loaded with dust and gases. Even if the “Rosetta mission” is postponed, with the consequence of a target change, we think that our idea and the method used for the simulations can be useful also for the new Rosetta target - the comet 67P/Churyumov Gerasimenko.

Published
2003
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66. Models of P/Borrelly: Activity and dust mantle formation

Author

Maria Teresa Capria, Angioletta Coradini, and M. C. De Sanctis

Subjects
Physics, Atmospheric Science, Complex topography, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, Mantle (geology), Geophysics, medicine.anatomical_structure, Space and Planetary Science, Comet nucleus, medicine, General Earth and Planetary Sciences, Nucleus
Abstract

Comet 19P/Borrelly was observed by Deep Space One spacecraft on September 22, 2001 (Soderblom et al., 2002).The DS1 images show a very dark and elongate nucleus with a complex topography; the IR spectra show a strong red-ward slope consistent with a very hot and dry surface (345K to 300K). During DS1 encounter the comet coma was dominated by a prominent jet but most of the comet was inactive, confirming the Earth-based observations that

Published
2003
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67. Modelling of cometary nuclei: Planetary missions preparation

Author

Maria Teresa Capria, Angioletta Coradini, and M. C. De Sanctis

Subjects
Physics, Atmospheric Science, Range (particle radiation), Comet, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, Crust, Planetary missions, Astrobiology, Geophysics, Space and Planetary Science, Thermal, Orbit (dynamics), General Earth and Planetary Sciences
Abstract

The planning of planetary missions requires the knowledge as much as possible accurate of the target. This knowledge, which cannot be obtained only by ground based observations, can be supported by theoretical modeling. This is particularly true in the case of Rosetta, a cornerstone ESA mission that will be launched in January 2003, and of its target, the comet 46P/Wirtanen. In this paper we show how, using a nucleus thermal evolution model, it is possible to foresee the temperature of the nucleus surface and the activity level along the orbit and define the range of possible values for these properties. Activity level close to the aphelion depends on the presence of CO. Surface temperatures depend on the physical properties attributed to the dust: temperatures reached by a crust mainly composed by silicatic grains differ from the temperatures reached by a crust mainly composed by organic grains.

Published
2003
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68. The organic-rich surface of comet 67P/Churyumov-Gerasimenko as seen by VIRTIS/Rosetta

Author

Gabriele Arnold, Maria Teresa Capria, Y. Hello, Kathrin Markus, Vincenzo Orofino, A. Semery, Romolo Politi, Stéphane Erard, Roberto Orosei, Robert W. Carlson, Davide Grassi, M. Combes, J. Crovisier, Gianfranco Magni, Andrea Raponi, Michael R. Combi, Priscilla Cerroni, Yves Langevin, L. Moroz, Pierre Drossart, Ulrich Schade, G. P. Tozzi, Wing-Huen Ip, Luigi Colangeli, Fredric W. Taylor, Angioletta Coradini, J. Ph. Combe, Raffaella Noschese, Enrico Flamini, Giancarlo Bellucci, Ernesto Palomba, Sonia Fornasier, F. Merlin, Lydie Bonal, Andrea Longobardo, G. Peter, M. Cartacci, Alessandro Frigeri, Giuseppe Piccioni, Bernard Schmitt, Uwe Fink, Ralf Jaumann, Mauro Ciarniello, D. Despan, M. A. Barucci, Giovanna Rinaldi, Pierre Beck, M. C. De Sanctis, S. Giuppi, S. Jacquinod, Uri Carsenty, D. Bockelee-Morvan, Eric Quirico, Stefano Mottola, F. Henry, N. Biver, Jean-Pierre Bibring, Patrick G. J. Irwin, T. Encrenaz, Katrin Stephan, Andrea Cicchetti, Johannes Benkhoff, C. Leyrat, Gianrico Filacchione, D. Tiphene, J. M. Reess, T. B. McCord, Sergio Fonti, Costanzo Federico, Eleonora Ammannito, M. I. Blecka, Pasquale Palumbo, Armando Blanco, M. Gudipati, Fabrizio Capaccioni, Vito Mennella, Federico Tosi, E. Kuehrt, F., Capaccioni, A., Coradini, G., Filacchione, S., Erard, G., Arnold, P., Drossart, M. C., De Sancti, D., Bockelee Morvan, M. T., Capria, F., Tosi, C., Leyrat, B., Schmitt, E., Quirico, P., Cerroni, V., Mennella, A., Raponi, M., Ciarniello, T., Mccord, L., Moroz, E., Palomba, E., Ammannito, M. A., Barucci, G., Bellucci, J., Benkhoff, J. P., Bibring, Blanco, Armando, M., Blecka, R., Carlson, U., Carsenty, L., Colangeli, M., Combe, M., Combi, J., Crovisier, T., Encrenaz, C., Federico, U., Fink, Fonti, Sergio, W. H., Ip, P., Irwin, R., Jaumann, E., Kuehrt, Y., Langevin, G., Magni, S., Mottola, Orofino, Vincenzo, P., Palumbo, G., Piccioni, U., Schade, F., Taylor, D., Tiphene, G. P., Tozzi, P., Beck, N., Biver, L., Bonal, Combe, J. P. h., D., Despan, E., Flamini, S., Fornasier, A., Frigeri, D., Grassi, M., Gudipati, A., Longobardo, K., Marku, F., Merlin, R., Orosei, G., Rinaldi, K., Stephan, M., Cartacci, A., Cicchetti, S., Giuppi, Y., Hello, F., Henry, S., Jacquinod, R., Noschese, G., Peter, R., Politi, J. M., Ree, A., Semery, Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), 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), Polska Akademia Nauk (PAN), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, German Aerospace Center (DLR), Department of Physics [Imperial College London], Imperial College London, Instituto de Estudos Avançados (IEAV), Institut, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Dipartimento di Fisica, Università degli studi di Lecce, Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], DLR Institute of Planetary Research, Department of Physics [Lecce], Università del Salento [Lecce], INAF - Osservatorio Astrofisico di Arcetri (OAA), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Alenia Aerospazio, JDS Uniphase/Cronos, USA, JDS Uniphase/Cronos, CNR-IASF, IASI (IASI), Istituti di Ricovero e Cura a Carattere Scientifico (IRCCS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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 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), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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), Polska Akademia Nauk = Polish Academy of Sciences (PAN), NASA-California Institute of Technology (CALTECH), University of Oxford, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ITA, USA, GBR, FRA, DEU, TWN, NLD, and POL

Subjects
67P/Churyumov-Gerasimenko, 010504 meteorology & atmospheric sciences, Opacity, Rosetta mission, VIRTIS, comets, Infrared, Comet, Imaging spectrometer, Astrophysics, 01 natural sciences, Astrobiology, comet, 0103 physical sciences, Spectral slope, Thermal, Rosetta, Rosetta mission, comets, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Multidisciplinary, Chemistry, Albedo, VIRTIS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], organic-rich
Abstract

The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 ± 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% kÅ −1 ), and the broad absorption feature in the 2.9-to-3.6–micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.

Published
2015
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69. Ammoniated phyllosilicates with a likely outer Solar System origin on (1) Ceres

Author

Ernesto Palomba, Fabrizio Capaccioni, Gianfranco Magni, Mauro Ciarniello, Filippo Giacomo Carrozzo, Federico Tosi, Ralf Jaumann, M. C. De Sanctis, Carol A. Raymond, J. P. Combe, Marco Giardino, Diego Turrini, Alessandro Frigeri, T. B. McCord, Francesca Zambon, Maria Teresa Capria, Harry Y. McSween, Carle M. Pieters, William C. Feldman, E. Ammannito, Sergio Fonte, Simone Marchi, Andrea Raponi, Michael J. Toplis, Thomas H. Prettyman, Lucy A. McFadden, Andrea Longobardo, Michelangelo Formisano, and Christopher T. Russell

Subjects
Solar System, Multidisciplinary, Materials science, Brucite, Dwarf planet, Mineralogy, engineering.material, ammoniated phyllosilicates, Astrobiology, Planetengeologie, Asteroid, Chondrite, engineering, Asteroid belt, Ceres, Clay minerals, Water vapor
Abstract

This article is in the 99th percentile (ranked 308th) of the 357,891 tracked articles of a similar age in all journals and the 94th percentile (ranked 54th) of the 934 tracked articles of a similar age in Nature. In the top 5% of all research outputs scored by Altmetric Studies of the dwarf planet (1) Ceres using ground-based and orbiting telescopes have concluded that its closest meteoritic analogues are the volatile-rich CI and CM carbonaceous chondrites. Water in clay minerals, ammoniated phyllosilicates, or a mixture of Mg(OH)2 (brucite), Mg2CO3 and iron-rich serpentine have all been proposed to exist on the surface. In particular, brucite has been suggested from analysis of the mid-infrared spectrum of Ceres. But the lack of spectral data across telluric absorption bands in the wavelength region 2.5 to 2.9 micrometres—where the OH stretching vibration and the H2O bending overtone are found—has precluded definitive identifications. In addition, water vapour around Ceres has recently been reported, possibly originating from localized sources. Here we report spectra of Ceres from 0.4 to 5 micrometres acquired at distances from ~82,000 to 4,300 kilometres from the surface. Our measurements indicate widespread ammoniated phyllosilicates across the surface, but no detectable water ice. Ammonia, accreted either as organic matter or as ice, may have reacted with phyllosilicates on Ceres during differentiation. This suggests that material from the outer Solar System was incorporated into Ceres, either during its formation at great heliocentric distance or by incorporation of material transported into the main asteroid belt.

Published
2015

70. Asteroid Thermophysical Modeling

Author

Marco Delbo, Ben Rozitis, Maria Teresa Capria, Michael Mueller, and Joshua P. Emery

Subjects
Thermal infrared, Spacecraft, Meteoroid, Field (physics), Infrared, business.industry, Albedo, Space exploration, Astrobiology, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Geology
Abstract

The field of asteroid thermophysical modeling has experienced an extraordinary growth in the last ten years, as new thermal infrared data became available for hundreds of thousands of asteroids. The infrared emission of asteroids depends on the body’s size, shape, albedo, thermal inertia, roughness and rotational properties. These parameters can therefore be derived by thermophysical modeling of infrared data. Thermophysical modeling led to asteroid size estimates that were confirmed at the few-percent level by later spacecraft visits. We discuss how instrumentation advances now allow mid-infrared interferometric observations as well as high-accuracy spectro-photometry, posing their own set of thermal-modeling challenges. We present major breakthroughs achieved in studies of the thermal inertia, a sensitive indicator for the nature of asteroids soils, allowing us, for instance, to determine the grain size of asteroidal regoliths. Thermal inertia also governs non-gravitational effects on asteroid orbits, requiring thermophysical modeling for precise asteroid dynamical studies. The radiative heating of asteroids, meteoroids, and comets from the Sun also governs the thermal stress in surface material; only recently has it been recognized as a significant weathering process. Asteroid space missions with thermal infrared instruments are currently undergoing study at all major space agencies. This will require a high level of sophistication of thermophysical models in order to analyse high-quality spacecraft data.

Published
2015
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71. IDIS Small Bodies and Dust Node: Technical innovation and science

Author

Diego Turrini, Lorenza Giacomini, Marco Giardino, Maria Teresa Capria, M. C. De Sanctis, S. Giuppi, V. F. Braga, and ITA

Subjects
Physics, Atmospheric Science, Service (systems architecture), Focus (computing), SIMPLE (military communications protocol), Node (networking), Aerospace Engineering, Astronomy and Astrophysics, Virtual observatory, Data science, Geophysics, Space and Planetary Science, Technical innovation, Information system, General Earth and Planetary Sciences, Remote sensing, Cosmic dust
Abstract

This work was supported by the EUROPLANET RI FP7 grant agreement 228319 It is not trivial, nowadays, to be fully aware of the impressive amount of astrophysical resources that are at hand. Virtual Observatories (VOs) were therefore created to provide a simple access to what astronomers look for. In this paper we focus on the original data access services developed specifically, in a VO perspective, for the "Small Bodies and Dust Node" (SBDN) in the framework of the Integrated and Distributed Information System (IDIS) initiative of the Europlanet Research Infrastructure project. We describe the scientific goals, along with the innovative technical aspects, of the tools that SBDN presently provides to the scientific community, namely the Comet Emission Lines service, and the Cosmic Dust Catalog service. In the former, an algorithm for the detection of unidentified emission lines has been implemented.

Published
2015

72. Separation of thermal inertia and roughness effects from Dawn/VIR measurements of Vesta surface temperatures in the vicinity of Marcia Crater

Author

Carol A. Raymond, Stephen Keihm, Federico Tosi, Andrea Longobardo, Maria Teresa Capria, Ernesto Palomba, Christopher T. Russell, M. C. De Sanctis, ITA, and USA

Subjects
Solar System, Thermal conductivity, Materials science, Impact crater, Space and Planetary Science, Asteroid, Mineralogy, Flux, Astronomy and Astrophysics, Surface finish, Granular material, Regolith, Astrobiology
Abstract

A physical model of small scale roughness has been applied to the analyses of VIR (Visible InfraRed mapping spectrometer) – measured surface temperatures in the Marcia Crater region of asteroid Vesta. Model-generated surface temperatures which include the effects of minicrater-induced flux enhancements and viewing geometry are compared with the measured surface temperature dependence on solar incidence and emission angles. Results indicate that an extremely low thermal inertia ( I = −1 m −2 s −1/2 ) and high roughness (rms slopes ∼35°) characterizes almost all of the areas in and around Marcia Crater. The one clear exception is the relatively cool pitted terrain region within Marcia Crater which requires either a higher thermal inertia value ( I ∼ 10) or significantly less roughness to match the VIR data. The I ∼ 5 finding is the lowest value found for the regolith of any airless body in the inner Solar System and is difficult to reproduce in either laboratory measurements or theoretical models of the thermal conductivity of dry granular materials in vacuum.

Published
2015

73. A model of the activity of comet wild 2

Author

M. C. De Sanctis, Maria Teresa Capria, and Angioletta Coradini

Subjects
Atmospheric Science, Materials science, Aerospace Engineering, Sintering, Astronomy and Astrophysics, Conductivity, Microstructure, Mantle (geology), Astrobiology, Geophysics, Thermal conductivity, Flux (metallurgy), Space and Planetary Science, Thermal, General Earth and Planetary Sciences
Abstract

A numerical model of the thermal evolution and chemical differentiation of cometary nuclei was developed to help in the preparation of future comet missions. To better describe the microstructure of cometary matter we modified the way in which bulk thermal conductivity is expressed. The matter is now described as an aggregate of grains, formed by a refractory core and an ice mantle. In this way the evolution of the microstructure due to various physical processes, such as sintering, can be better simulated. With this kind of formulation, bulk conductivity could be very low, orders of magnitude lower than in our previous versions of the model. In order to test this expression and its consequences, we present here a simulation of the thermal evolution of comet Wild 2, the target of the STARDUST mission. We can see that a much lower conductivity changes the internal stratigraphy and the flux of low volatile gases, but does not affect surface properties and consequently water and dust fluxes.

Published
2002
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74. Planetary Science Virtual Observatory architecture

Author

P. Le Sidaner, Gérard Chanteur, Maria Teresa Capria, Stéphane Erard, Bernard Schmitt, Vincent Génot, M. Gangloff, C. Chauvin, Jérôme Berthier, N. André, C. Jacquey, Baptiste Cecconi, F. Henry, N. Bourrel, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL), Centre d'étude spatiale des rayonnements (CESR), 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), Institut de recherche en astrophysique et planétologie (IRAP), 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 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-École polytechnique (X)-Sorbonne Universités-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Virtual observatory, 01 natural sciences, Field (computer science), [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 0103 physical sciences, Architecture, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Planetary Sciences, Astronomy and Astrophysics, Virtual Observatory, Computer Science Applications, Planetary science, Space and Planetary Science, Systems engineering, Data as a service, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; In the framework of the Europlanet-RI program, a prototype of Virtual Observatory dedicated to Planetary Science was defined. Most of the activity was dedicated to the elaboration of standards to retrieve and visualize data in this field, and to provide light procedures to teams who wish to contribute with on-line data services. The architecture of this VO system and selected solutions are presented here, together with existing demonstrators.

Published
2014
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75. Thermal Evolution and Differentiation of Edgeworth–Kuiper Belt Objects

Author

Maria Teresa Capria, Angioletta Coradini, and M. C. De Sanctis

Subjects
Physics, Solar System, Radiogenic nuclide, business.industry, Nice model, Astronomy, Astronomy and Astrophysics, Solar energy, Astrobiology, Space and Planetary Science, Neptune, Asteroid, Trans-Neptunian object, Formation and evolution of the Solar System, business
Abstract

The region beyond Neptune's orbit is populated by numerous bodies with semimajor axes from 31 to 48 AU. This region, known as the Kuiper belt, should contain primitive bodies, perhaps among the most primitive objects in the solar system. These bodies could be remnants of the solar system formation. They seem to be dark, volatile-rich objects showing a strong relationship with comets: the Kuiper belt is probably the source of most short-period comets and Centaurs. The Kuiper belt objects (KBOs) could still contain ices and organic compounds in unaltered proportions with respect to those of their formation. Thermal models of bodies moving in Kuiper belt orbits have been developed to follow their evolution and differentiation and to better understand the relations between them and the short-period comets and Centaurs. In these models, we assume that KBOs are porous bodies composed of ices and dust. The solar energy is very low, between 30 and 50 AU, and radiogenic heating becomes a nonnegligible source of energy for differentiation. The radioactive elements, if they exist in sufficient quantity, may modify the original composition of cometary nuclei. In the models reported here, we have assumed that the radiogenic elements stored in the refractory component are 40K, 232Th,235U, and 238U, in meteoritic proportions. In some models, we have also included the short-lived radio nuclide 26Al. The aim of this work is to see how an undifferentiated Kuiper belt body can change its internal structure under the combined effect of radiogenic heating and solar irradiation. Moderate heating can permit the sublimation of the most volatile ices both from the interior and from the surface, depending on the dominant heat source. The main result is that Kuiper belt objects can be strongly volatile depleted. From the surface down to several hundred meters below the surface, the most volatile ices (like CO) can be completely absent.

Published
2001
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76. MARS-IRMA: in-situ infrared microscope analysis of Martian soil and rock samples

Author

S. Espinasse, Maria Teresa Capria, Carle M. Pieters, M. DiGiampietro, John F. Mustard, Angioletta Coradini, Sergio Fonti, Olivier Forni, M. Poscolieri, R. Bianchi, Vittorio Formisano, Roberto Orosei, Fabrizio Capaccioni, C Pasqui, M. Magnani, E. Battistelli, A. Romoli, M. I. Blecka, S. Amici, Giuseppe Piccioni, Stéphane Erard, and Giancarlo Bellucci

Subjects
Martian, Atmospheric Science, Aerospace Engineering, Hyperspectral imaging, Astronomy and Astrophysics, Weathering, Mars Exploration Program, Martian soil, Present day, Astrobiology, Petrography, Geophysics, Space and Planetary Science, Martian surface, General Earth and Planetary Sciences, Environmental science, Remote sensing
Abstract

IRMA (the acronym stands for InfraRed Microscope Analysis) is a hyperspectral imaging spectrometer which is capable, in its present design, to achieve a spatial resolution of 38 μm in the 0.8–5 μm infrared spectral range. IRMA has the goal to first ever quantitatively characterize the mineralogy and the microphysical structure of the materials of the Martian soils and rocks down to the depth available to a lander sampling mechanism. The experiment has been selected by the Italian Space Agency (ASI), in the framework of the Italian participation to the NASA's Mars Surveyor Programme, to be part of the Italian Package for Scientific Experiments (IPSE). IPSE was to fly on-board the ill-fated MARS2003 MARS SAMPLE RETURN Mission, postponed during the early months of 2000 to a later date (possibly 2007). IRMA present state of development is compatible with a flight readiness in 2007. IPSE is a small laboratory devoted to the analysis of in situ collected samples of rock and soil of Martian material. Details on IPSE are given in a paper in this same journal issue. IRMA will provide detailed information on: • texture, habit and microphysical properties of the grains and particulates of the Martian soil as well as the petrography of Martian rocks, with a spatial resolution of the order of the tens of micron. • Mineralogical composition and relative mineral abundances of the rocks and soils, with a relative accuracy of the order of 1%. A Signal to Noise Ratio of at least 100 shall be required to achieve this goal IRMA measurements shall provide essential contributions to the understanding of outstanding scientific issues such as the history of water and other volatiles, e.g., CO2, the role of physical and chemical weathering in the past and present day Mars and hence the assessment of the environmental conditions present on the martian surface throughout its history.

Published
2001
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77. Thermal Evolution of the Centaur Object 5145 Pholus

Author

Roberto Orosei, M. C. De Sanctis, Angioletta Coradini, and Maria Teresa Capria

Subjects
Physics, Organic dust, Space and Planetary Science, Asteroid, Thermal, Orbit (dynamics), Object (grammar), Astronomy, Astronomy and Astrophysics, Class (philosophy), Trans-Neptunian object, Astrophysics, Centaur
Abstract

We present the results obtained by the simulations of different thermal models of 5145 Pholus, one of the known Centaurs. Pholus's orbit is highly eccentric, similar to that of comets, but its dimension is more similar to larger asteroids. Pholus cannot be clearly numbered in either class. The most likely source of Centaurs is the Edgeworth-Kuiper belt: dynamical studies and physical properties suggest that Pholus recently entered the planetary zone. Here we assume that the nature of Pholus is that of a cometary body made of different ices and dust. We have computed the thermal evolution of this object under different conditions: as a "new" object, namely an undifferentiated body, and an "old" one, differentiated and aged in the Kuiper belt. We have tried to see also the effects induced by the presence of an organic dust on the overall evolution. Both the "new" and the "old" object show low, but different, levels of gas activity.

Published
2000
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78. Results from the comet nucleus model team at the international space science institute, Bern, Switzerland

Author

Johannes Benkhoff, Roberto Orosei, Dina Prialnik, Walter F. Huebner, Angioletta Coradini, A Enzian, M. C. De Sanctis, and Maria Teresa Capria

Subjects
Physics, Atmospheric Science, Code development, Meteorology, Aerospace Engineering, Astronomy and Astrophysics, Mantle (geology), Computational physics, Geophysics, Space and Planetary Science, Comet nucleus, General Earth and Planetary Sciences, Water ice, Space Science
Abstract

Five one-dimensional algorithms for heat and gas transport in porous icy bodies have been applied, each to four simplified compositions of comet nucleus models: (1) pure H 2 O ice, (2) a mixture of H 2 O and CO ices, (3) a mixture of H 2 O ice and dust, and (4) a mixture of H 2 O and CO ices and dust. In addition, two different pore radii were assumed in models 3 and 4. The algorithms were chosen on the basis of recent applications and independent code development and evolution. A sixth algorithm was used only in a few models. Results for a spinning comet nucleus in the orbit of Comet 46P/Wirtanen were compared to establish credibility for the five algorithms. Discrepancies in results were discussed and isolated for possible causes. The algorithms were then investigated and modified by the presenting team members. After resolutin of major differences from the simple models, each team member will be able to address more complex models of their own choosing with greater confidence. These models will include investigations of the effects of amorphous versus crystalline water ice, trapped gases versus frozen gases, multi-dimensional calculations, and dust mantle development and removal. Results and progress on the algorithms, and plans for further development are discussed.

Published
1999
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79. Compositional evidence of magmatic activity on Vesta

Author

Francesca Zambon, Debra Buczkowski, Fabrizio Capaccioni, Eleonora Ammannito, D. W. Mittlefehldt, Gianfranco Magni, Federico Tosi, Maria Teresa Capria, Ralf Jaumann, Alessandro Frigeri, Christopher T. Russell, Carol A. Raymond, and M. C. De Sanctis

Subjects
Basalt, asteroids, geography, volcanism, geography.geographical_feature_category, protoplanet, solar system origin, Crust, Astrobiology, Planetengeologie, Vesta, Geophysics, Impact crater, Meteorite, Volcano, Asteroid, General Earth and Planetary Sciences, Ejecta, Protoplanet, Geology
Abstract

Like the Earth and other terrestrial planets, the asteroid Vesta has a basaltic crust and a large iron core; its surface is dominated by impact craters of all sizes and has tectonic features. The presence of basaltic compositions, olivine, howardite-eucrite-diogenite meteorites, and models of Vesta's formation, suggests that volcanic and/or magmatic activity could have occurred on Vesta. A global search for lobate structures did not find unequivocal evidence of volcanic features. Nevertheless, several morphological properties of Brumalia Tholus on Vestalia Terra suggest that this topographic high most likely formed as a magmatic intrusion. The presence of more orthopyroxene-rich material relative to surrounding terrain in the ejecta of Teia, a fresh impact crater on the northern face of Brumalia Tholus, supports the hypothesis of magmatic intrusions on Vesta.

Published
2014

80. Thermal measurements of dark and bright surface features on Vesta as derived from Dawn/VIR

Author

J. M. Sunshine, Fabrizio Capaccioni, Andrea Longobardo, Stefan Schröder, J. Ph. Combe, Carol A. Raymond, David T. Blewett, Andreas Nathues, Federico Tosi, D. W. Mittlefehldt, Maria Teresa Capria, Jian-Yang Li, Eric Palmer, T.M. Titus, Ernesto Palomba, M. C. De Sanctis, Eleonora Ammannito, Christopher T. Russell, Brett W. Denevi, and Francesca Zambon

Subjects
Physics, Spectrometer, Infrared observations, Infrared, Astronomy, Astronomy and Astrophysics, Albedo, surfaces, Asteroids, Meteorite, Space and Planetary Science, Spectrophotometry, Solar time, Thermal, Emissivity, Ejecta, Asteroid Vesta
Abstract

Remote sensing data acquired during Dawn’s orbital mission at Vesta showed several local concentrations of high-albedo (bright) and low-albedo (dark) material units, in addition to spectrally distinct meteorite impact ejecta. The thermal behavior of such areas seen at local scale (1–10 km) is related to physical properties that can provide information about the origin of those materials. We use Dawn’s Visible and InfraRed (VIR) mapping spectrometer hyperspectral data to retrieve surface temperatures and emissivities, with high accuracy as long as temperatures are greater than 220 K. Some of the dark and bright features were observed multiple times by VIR in the various mission phases at variable spatial resolution, illumination and observation angles, local solar time, and heliocentric distance. This work presents the first temperature maps and spectral emissivities of several kilometer-scale dark and bright material units on Vesta. Results retrieved from the infrared data acquired by VIR show that bright regions generally correspond to regions with lower temperature, while dark regions correspond to areas with higher temperature. During maximum daily insolation and in the range of heliocentric distances explored by Dawn, i.e. 2.23–2.54 AU, the warmest dark unit found on Vesta rises to a temperature of 273 K, while bright units observed under comparable conditions do not exceed 266 K. Similarly, dark units appear to have higher emissivity on average compared to bright units. Dark-material units show a weak anticorrelation between temperature and albedo, whereas the relation is stronger for bright material units observed under the same conditions. Individual features may show either evanescent or distinct margins in the thermal images, as a consequence of the cohesion of the surface material. Finally, for the two categories of dark and bright materials, we were able to highlight the influence of heliocentric distance on surface temperatures, and estimate an average temperature rate change of 1% following a variation of 0.04 AU in the solar distance.

Published
2014

81. Spectral analysis of the bright materials on the asteroid Vesta

Author

Carle M. Pieters, Carol A. Raymond, Fabrizio Capaccioni, Alessandro Frigeri, David W. Mittlefehldt, Andrea Longobardo, Federico Tosi, Jian-Yang Li, Ernesto Palomba, Christopher T. Russell, Francesca Zambon, David T. Blewett, Stefan Schröder, Maria Teresa Capria, Maria Cristina De Sanctis, Sergio Fonte, Eleonora Ammannito, and Andreas Nathues

Subjects
Eucrite, Diogenite, Howardite, Astronomy and Astrophysics, Pyroxene, Astrophysics, Albedo, Mineralogy, Spectral line, Astrobiology, Meteorite, Space and Planetary Science, Asteroid, Asteroid Vesta, Geology, Spectroscopy
Abstract

Vesta spectra have prominent near-infrared absorption bands characteristic of pyroxenes, indicating a direct link to the howardite, eucrite and diogenite meteorites. Many localized dark and bright materials are present on Vesta’s surface. Here we focus on the bright material (BM) units to determine their spectral properties, their origin, the presence of mineralogical phases different from pyroxenes, and whether different bright units share a common lithology. VIR, the Visible and Infrared spectrometer onboard Dawn, allows us to first do a detailed analysis of the spectral properties of a large number of bright material units on Vesta including examples of the different morphological classes. The spectral parameters used are band centers, band depths, and Band Area Ratio (BAR) for the pyroxene bands at ∼0.9 and ∼1.9 μm. The mineralogies of most bright regions are consistent with those of the howardite, eucrite and diogenite meteorites typical of Vesta’s surface. We find that bright material units exhibit the full range of HED pyroxene composition, from eucrites to diogenites. Large part of the bright materials are eucrite-rich, according with the Vesta’s mineralogy. In most cases, the bright materials have the same mineralogy of the surrounding terrain, but have larger band depth values. The band depths can be related to the abundance of the absorbing minerals, the abundance of Fe2+, grain size, and/or to the abundance of opaque materials. We found a positive correlation between albedo and band depth, which suggests that the grain size is not the main factor responsible for the higher albedo. The analysis of the band parameters indicates that most of the bright materials, excluding the few olivine-rich units, represent fresh uncontaminated Vestan pyroxenes from a variety of lithologies exposed from beneath the surface by impacts.

Published
2014

82. Composition and mineralogy of dark material units on Vesta

Author

Andrea Longobardo, Francesca Zambon, Carol A. Raymond, Federico Tosi, Fabrizio Capaccioni, Ernesto Palomba, Ralf Jaumann, Edward A. Cloutis, Maria Teresa Capria, Christopher T. Russell, Maria Cristina De Sanctis, Eleonora Ammannito, Alessandro Frigeri, and Jean-Philippe Combe

Subjects
Solar System, Imaging spectrometer, Astronomy, Astronomy and Astrophysics, Context (language use), Albedo, surfaces, Mineralogy, Regolith, Spectral line, Asteroids, Planetengeologie, Space and Planetary Science, Chondrite, Asteroid, Regoliths, Asteroid Vesta, Geology, Spectroscopy
Abstract

Vesta is the asteroid with the largest albedo variation among the known rocky Solar System objects and shows a widespread occurrence of dark material (DM) and bright material (BM) units. In the first observation phases by the Dawn spacecraft, two main extensions of low albedo areas were identified on Vesta and found to be closely correlated with carbonaceous, OH-rich, material. In this work we use the hyperspectral data provided by the VIR-Dawn imaging spectrometer onboard Dawn to detect and analyze individual, well-defined, dark material units. We define {DM} units assuming a relative criterion, i.e. reflectance lower than the surroundings. By coupling visible and infrared images of the same area we are able to select real dark material units, discarding false detections created by shadowing effects. A detailed final catalogue of 123 dark units is presented, containing the geographical parameters and the main spectral characteristics for each unit. Independently of the geological context of the dark units, all {DMs} show similar spectral properties, dominated by the pyroxene absorption features, as is the average spectrum of Vesta. This finding suggests a similar composition, with the presence of darkening agents that also weaken pyroxene band depths. The majority (90) of the {DM} units shows a positive correlation between low albedo and an {OH} band centered at 2.8 μm, confirming the hypothesis that the darkening agents are carbonaceous chondrites, probably delivered by low-velocity impacts of primitive asteroids. A comparison with laboratory spectra allows us to better constrain the size and the composition of the darkening agents. These {DM} areas seem to be made of eucritic material. The regolith grain size seems to be nearly constant around an average value of 25 μm, and is quite homogenous at least in the first hundreds of meters beneath the Vesta surface, suggesting similar processing mechanisms for both {DM} and BM.

Published
2014

83. Spectroscopic Characterization of Mineralogy and Its Diversity Across Vesta

Author

Maria Teresa Capria, Federico Tosi, T. B. McCord, Gianfranco Magni, Sergio Fonte, Ernesto Palomba, Francesca Zambon, Carol A. Raymond, Christopher T. Russell, F. Carraro, Fabrizio Capaccioni, Ralf Jaumann, M. C. De Sanctis, Eleonora Ammannito, David W. Mittlefehldt, Alessandro Frigeri, Carle M. Pieters, Andreas Nathues, Simone Marchi, Diego Turrini, Michael J. Toplis, Lucy A. McFadden, and Harry Y. McSween

Subjects
Basalt, Eucrite, Diogenite, Multidisciplinary, Howardite, Mineralogy, Crust, Mantle (geology), Dawn, Vesta, Impact crater, mineralogy, Ejecta, Geology
Abstract

A New Dawn Since 17 July 2011, NASA's spacecraft Dawn has been orbiting the asteroid Vesta—the second most massive and the third largest asteroid in the solar system (see the cover). Russell et al. (p. 684 ) use Dawn's observations to confirm that Vesta is a small differentiated planetary body with an inner core, and represents a surviving proto-planet from the earliest epoch of solar system formation; Vesta is also confirmed as the source of the howardite-eucrite-diogenite (HED) meteorites. Jaumann et al. (p. 687 ) report on the asteroid's overall geometry and topography, based on global surface mapping. Vesta's surface is dominated by numerous impact craters and large troughs around the equatorial region. Marchi et al. (p. 690 ) report on Vesta's complex cratering history and constrain the age of some of its major regions based on crater counts. Schenk et al. (p. 694 ) describe two giant impact basins located at the asteroid's south pole. Both basins are young and excavated enough amounts of material to form the Vestoids—a group of asteroids with a composition similar to that of Vesta—and HED meteorites. De Sanctis et al. (p. 697 ) present the mineralogical characterization of Vesta, based on data obtained by Dawn's visual and infrared spectrometer, revealing that this asteroid underwent a complex magmatic evolution that led to a differentiated crust and mantle. The global color variations detailed by Reddy et al. (p. 700 ) are unlike those of any other asteroid observed so far and are also indicative of a preserved, differentiated proto-planet.

Published
2012
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84. Europlanet-IDIS Data model: a Data Model for a Planetology Virtual Observatory

Author

Baptiste Cecconi, Jean Aboudarham, Nicolas André, Jérôme Berthier, Natacha Bourrel, Maria Teresa Capria, Maria Cristina de Sanctis, Stéphane Erard, Michel Gangloff, Christian Jacquey, Maxim Khodachenko, Pierre Le Sidaner, Cédric Leyrat, Nicolas Manaud, Walter Schmidt, Bernard Schmitt, Florian Topf, Frank Trauthan, Alain Sarkissian, Sandrine Vinatier, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Finnish Meteorological Institute (FMI), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), PLANETO - LATMOS, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and 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)

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

International audience; IDIS (Integrated and Distributed Information System) is part of the Europlanet project and aims to develop a prototype of a planetology Virtual Observatory. In the frame of its participation to this project, the CDPP (Data Centre for Plasma Physics, based in Toulouse) is developing a new data model to describe the wide variety of data products that can be found in the planetology community, which includes a wide variety of science thematics such as plasma physics, planetary surfaces, interiors, atmospheres or small bodies. This data model is making extensive use of existing standards provided by various groups (IVOA, SPASE...). The scope of this data model is to describe the scientific content of the data sets, in order to be able to locate and retrieve the data files corresponding to a given request. The initial version has been developed to describe plasma data, which can be very heterogeneous (time series, spectra, dynamic spectra, maps...). Two models are tested in collaboration with VO-Paris (Virtual Observatory Paris Data Centre) and other Europlanet IDIS partners in order to take into account characteristics of data from other thematics of planetary sciences.

Published
2011

85. The Surface Composition and Temperature of Asteroid 21 Lutetia As Observed by Rosetta/VIRTIS

Author

Maria Teresa Capria, M. Combes, G. Neukum, Johannes Benkhoff, Stefano Mottola, Pierre Drossart, Uwe Fink, D. Bockelee-Morvan, Vincenzo Orofino, R. W. Carlson, E. T. Encrenaz, M. C. De Sanctis, Davide Grassi, Uri Carsenty, F. Carraro, Michael R. Combi, Luigi Colangeli, M. A. Barucci, Fabrizio Capaccioni, E. Kuehrt, Ralf Jaumann, S. Giuppi, J. Crovisier, Vito Mennella, Federico Tosi, Sergio Fonti, Eleonora Ammannito, D. Tiphene, Wing-Huen Ip, Gianfranco Magni, Fredric W. Taylor, Angioletta Coradini, Gianrico Filacchione, Costanzo Federico, Jean-Pierre Bibring, M. I. Blecka, Pasquale Palumbo, Armando Blanco, G. Arnold, Yves Langevin, Giuseppe Piccioni, Ulrich Schade, G. P. Tozzi, Bernard Schmitt, Lorenza Giacomini, Stéphane Erard, Priscilla Cerroni, Giancarlo Bellucci, T. B. McCord, Coradini, A., Blanco, Armando, Fonti, Sergio, Orofino, Vincenzo, and …., et al

Subjects
Mineral hydration, education.field_of_study, Multidisciplinary, Spectral signature, Materials science, Infrared, Population, Imaging spectrometer, Lutetia, Regolith, Space weathering, Astrobiology, Asteroid, Rosetta, education, Virtis
Abstract

The Visible, InfraRed, and Thermal Imaging Spectrometer (VIRTIS) on Rosetta obtained hyperspectral images, spectral reflectance maps, and temperature maps of the asteroid 21 Lutetia. No absorption features, of either silicates or hydrated minerals, have been detected across the observed area in the spectral range from 0.4 to 3.5 micrometers. The surface temperature reaches a maximum value of 245 kelvin and correlates well with topographic features. The thermal inertia is in the range from 20 to 30 joules meter(-2) kelvin(-1) second(-0.5), comparable to a lunarlike powdery regolith. Spectral signatures of surface alteration, resulting from space weathering, seem to be missing. Lutetia is likely a remnant of the primordial planetesimal population, unaltered by differentiation processes and composed of chondritic materials of enstatitic or carbonaceous origin, dominated by iron-poor minerals that have not suffered aqueous alteration.

Published
2011
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86. Thermal evolution and differentiation of a short-period comet

Author

M. Salomone, Costanzo Federico, Maria Teresa Capria, Roberto Orosei, Angioletta Coradini, S. Espinasse, and Fabrizio Capaccioni

Subjects
Materials science, Vapor pressure, Thermodynamic equilibrium, Comet, Thermodynamics, Astronomy and Astrophysics, Mechanics, Perfect gas, Thermal conduction, Space and Planetary Science, Sublimation (phase transition), Astrophysics::Earth and Planetary Astrophysics, Knudsen number, Physics::Atmospheric and Oceanic Physics, Water vapor
Abstract

The evolution of the subsurface layers of a short-period comet has been studied. The structure and composition of the surface layers due to sublimation recondensation phenomena, to gas diffusion processes through the pore system and to the ejection of dust particles have been investigated in detail. The nucleus has been modelled as a mixture of water ice, CO2 ice and dust in specified proportions. The icy matrix is assumed to be porous and crystalline. The model is based on the solution of two symmetric diffusion equations through the whole nucleus, one describing the transport of matter and the other the transport of heat. These equations are linked by a source term which accounts for production or loss of gas. We assume that the water vapour present in the pore system acts as a perfect gas, and that sublimation and recondensation are instantaneous in order to maintain the local thermodynamic equilibrium between the solid phase and its vapour. Under these assumptions, the source term depends on the variation of the pressure due to vapour diffusion, and on the variation of the saturation pressure of the vapour due to the evolution of the temperature. The diffusion regime, Knudsen or viscous, depends on the mean free path of the molecules of gas through the pore network, considered as a system of cylindrical pipes. The dust particles may be removed from the surface of the nucleus depending on the force balance. The calculations are performed for a nucleus on the orbit of P/Du Toit-Hartley, that was one of the possible targets for the Rosetta mission. Different nucleus compositions with various CO2/H2O ice and dust/ice ratios are investigated. Results are presented on the evolution of the stratigraphy of the nucleus and on the production rates of CO2. H2O and dust particles as a function of the heliocentric distance. Several phenomena are observed, such as the depletion of CO2 ice in the subsurface layers and the possible formation of a dust layer at the nucleus surface.

Published
1993
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87. SIMBIO-SYS: The spectrometer and imagers integrated observatory system for the BepiColombo planetary orbiter

Author

Francois Poulet, J. Ficai Veltroni, Carlo Bettanini, Stéphane Erard, M. Cosi, Maria Teresa Capria, Alessandro Caporali, Lorenza Giacomini, Maria Sgavetti, Giampiero Naletto, Luciano Calamai, Lucia Marinangeli, Luigi Colangeli, Yann Hello, Leonardo Tommasi, M. Dami, G. Marra, Costanzo Federico, P. Eng, Fabrizio Capaccioni, Yves Langevin, E. Mazzotta Epifani, Pasquale Palumbo, Elena Martellato, Gianrico Filacchione, Olivier Forni, Alain Doressoundiram, Enrico Flamini, V. Da Deppo, Jean-Luc Josset, Matteo Massironi, Mirco Zaccariotto, J.F. Roig, Gabriele Cremonese, Michele Zusi, Stefano Debei, M. C. De Sanctis, Agenzia Spaziale Italiana (ASI), Istituto di Astrofisica Spaziale e Fisica Cosmica (IASF-Roma), INAF-Osservatorio Astronomico di Capodimonte (INAF-OAC), INAF-Osservatorio Astronomico di Padova, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), SPACE-X, Space Exploration Institute, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Università degli Studi di Padova = University of Padua (Unipd), International Research School of Planetary Sciences, Dipartimento di Scienze, Università d'Annunzio, Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), CNR-INFM Luxor, Centre d'étude spatiale des rayonnements (CESR), 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), Università degli studi di Parma = University of Parma (UNIPR), and Galileo Avionica

Subjects
Spectrometer, BepiColombo, Imaging spectrometer, Astronomy and Astrophysics, Planetary geology, Mercury, law.invention, Orbiter, Stereo imaging, Mercury Surface composition BepiColombo SIMBIO-SYS Planetary geology, Space and Planetary Science, Planet, law, Observatory, Surface composition, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, Remote sensing, Exosphere, SIMBIO-SYS
Abstract

International audience; The limited knowledge about the majority of the Mercury surface leaves many open questions regarding its geological evolution, the anomalously high metal/silicate ratio, the magnetic field generation and exosphere evolution. An integrated suite of instruments, Spectrometer and Imagers for MPO BepiColombo-Integrated Observatory SYStem (SIMBIO-SYS), which includes a stereo imaging system (STC), a high-resolution imager (HRIC) and a visible-near-infrared imaging spectrometer (VIHI), has been selected for the ESA BepiColombo mission to Mercury. SIMBIO-SYS will scan the hermean surface with the three channels and map the physical, morphological, tectonic and compositional properties of the entire planet. The availability of high-resolution images will unveil details of specific target at an unprecedented resolution. The main scientific objectives and performances along with technical characteristics of SIMBIO-SYS are described in this paper.

Published
2010
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89. Modélisation de noyaux cométaires pour la préparation scientifique de la mission spatiale Rosetta

Author

Jérémie Lasue, Angioletta Coradini, Maria Cristina de Sanctis, Anny Chantal Levasseur-Regourd, Robert Botet, Maria Teresa Capria, Gianfranco Magni, Wlodek Kofman, Diego Turrini, Pibaret-Bourdon, Béatrice, Service d'aéronomie (SA), 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), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Solides (LPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Consiglio Nazionale delle Ricerche (CNR), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Published
2007

90. Virtis: An Imaging Spectrometer for the Rosetta Mission

Author

Uwe Fink, Bortolino Saggin, Sergio Fonti, Eleonora Ammannito, Costanzo Federico, Vittorio Formisano, M.C. Desanctis, M. I. Blecka, Pasquale Palumbo, Bernard Schmitt, Michael R. Combi, Antonella Barucci, Luigi Colangeli, Thomas B. McCord, Wing-Huen Ip, Heike Rauer, Maria Teresa Capria, Stéphane Erard, Gabriele Arnold, Gianrico Filacchione, Francesco Angrilli, G. Bianchini, Pierre Drossart, Jean-Pierre Bibring, Yves Langevin, Stefano Mottola, G. Neukum, Giulio Magni, E. T. Encrenaz, Angioletta Coradini, R. W. Carlson, G. P. Tozzi, Johannes Benkhoff, Uri Carsenty, M. Combes, E. Kuehrt, Giuseppe Piccioni, Priscilla Cerroni, Ralf Jaumann, Fabrizio Capaccioni, Vito Mennella, J. Crovisier, Dominique Bockelée-Morvan, Didier Tiphene, Giancarlo Bellucci, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), German Aerospace Center (DLR), Dipartimento di Ingegneria Meccanica, Università degli Studi di Padova = University of Padua (Unipd), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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)-Centre National d’Études Spatiales [Paris] (CNES), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), INAF - Osservatorio Astronomico di Capodimonte (OAC), Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Università degli Studi di Perugia = University of Perugia (UNIPG), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Dipartimento di Fisica, Università degli studi di Lecce, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universita degli Studi di Padova, 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), Polska Akademia Nauk (PAN), Università degli Studi di Perugia (UNIPG), Max-Planck-Institut für Sonnensystemforschung (MPS), and California Institute of Technology (CALTECH)-NASA

Subjects
spectroscopy, 010504 meteorology & atmospheric sciences, Comet, Imaging spectrometer, Context (language use), space mission, 01 natural sciences, 7. Clean energy, Space exploration, Comets, Space missions, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, Astrobiology, law.invention, Orbiter, law, 0103 physical sciences, comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Mars Exploration Program, space missions, Planetary science, 13. Climate action, Asteroid, Geology
Abstract

International audience; The VIRTIS (Visual IR Thermal Imaging Spectrometer) experiment has been one of the most successful experiments built in Europe for Planetary Exploration. VIRTIS, developed in cooperation among Italy, France and Germany, has been already selected as a key experiment for 3 planetary missions: the ESA-Rosetta and Venus Express and NASA-Dawn. VIRTIS on board Rosetta and Venus Express are already producing high quality data: as far as Rosetta is concerned, the Earth-Moon system has been successfully observed during the Earth Swing-By manouver (March 2005) and furthermore, VIRTIS will collect data when Rosetta flies by Mars in February 2007 at a distance of about 200 kilometres from the planet. Data from the Rosetta mission will result in a comparison – using the same combination of sophisticated experiments – of targets that are poorly differentiated and are representative of the composition of different environment of the primordial solar system. Comets and asteroids, in fact, are in close relationship with the planetesimals, which formed from the solar nebula 4.6 billion years ago. The Rosetta mission payload is designed to obtain this information combining in situ analysis of comet material, obtained by the small lander Philae, and by a long lasting and detailed remote sensing of the comet, obtained by instrument on board the orbiting Spacecraft. The combination of remote sensing and in situ measurements will increase the scientific return of the mission. In fact, the “in situ” measurements will provide “ground-truth” for the remote sensing information, and, in turn, the locally collected data will be interpreted in the appropriate context provided by the remote sensing investigation. VIRTIS is part of the scientific payload of the Rosetta Orbiter and will detect and characterise the evolution of specific signatures – such as the typical spectral bands of minerals and molecules – arising from surface components and from materials dispersed in the coma. The identification of spectral features is a primary goal of the Rosetta mission as it will allow identification of the nature of the main constituent of the comets. Moreover, the surface thermal evolution during comet approach to sun will be also studied.

Published
2007
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91. Deep Impact: Observations from a Worldwide Earth-Based Campaign

Author

Jean Manfroid, Miroslav Filipovic, Christiaan Sterken, Maria Teresa Capria, M. J. S. Belton, N. Ageorges, U.W. Kamath, L. M. Woodney, Randy D. Campbell, Tomohiko Sekiguchi, Diane H. Wooden, Tetsuharu Fuse, Nicholas B. Suntzeff, S.K. Pandea, Michael J. Mumma, Jacques Crovisier, Emmanuel Jehin, Itsuki Sakon, R. Fugate, H. U. Kaufl, D. Fong, L. Barrera, Anita L. Cochran, Ivo Saviane, Jeremy Bailey, K. von Braun, R. Barrena, G. Ruch, G. R. Stecklein, Sunao Hasegawa, Miquel Serra-Ricart, J. Watanabe, T. Carroll, Damien Hutsemekers, Brian M. Patten, Ronald L. Snell, R. G. Sharp, Takuya Fujiyoshi, S. Fisher, Geraint H. Jones, R. Cleis, Scott J. Wolk, Geoffrey A. Blake, Toshihiko Kadono, Susan M. Lederer, Michael F. A'Hearn, David J. Wilner, William F. Welsh, Daisuke Kinoshita, S.D. Rodgers, L. Dundon, J.-H. Wu, Marc W. Buie, Jianguo Li, Luisa Lara, Yanga R. Fernandez, Paul A. Jones, Wiphu Rujopakarn, Geronimo L. Villanueva, Michael G. Burton, Ramprasad Rao, Florian Kerber, Takaki Miyata, S. M. Larson, Stephen C. Lowry, Remi A. Cabanac, J. Debuizer, Richard J. Wainscoat, Paul R. Weissman, D. K. Sahu, Heike Rauer, Ellen S. Howell, T. Yamashita, Boncho P. Bonev, Stefano Bagnulo, G. P. Tozzi, Hideyo Kawakita, Tushar P. Prabhu, P. Colom, H. Tran, J. Aycock, Andrew J. Coates, Jack D. Drummond, Chick E Woodward, N. Biver, Harold A. Weaver, James E. Lyke, Bin Yang, Patrick Seitzer, Alan Fitzsimmons, Richard Dekany, Michael S. P. Kelley, Zhong-Yi Lin, Shigehisa Takakuwa, M. Sumner, Mark Gurwell, Rita Schulz, Harold J. Reitsema, Karen J. Meech, Bidushi Bhattacharya, Choogon Lee, Gerald Moriarty-Schieven, Samuel Gulkis, O. Marco, D. Harrington, Matthew M. Knight, David E. Harker, Roberto Vázquez, Olivier Hainaut, R. Swaters, M. Schirmer, Z.J. Jiang, X. Zhao, Fernando Selman, Humberto Campins, Tom Stallard, Maria Womack, Daisuke Iono, Noemi Pinilla-Alonso, Pierre Martin, E. Thompson, William M. Jackson, Alan T. Tokunaga, Bryan E. Penprase, Al Conrad, Amy J. Lovell, Mitsuhiko Honda, Rosemary Barber, A. C. Zook, David K. Lynch, A. Delsanti, Hermann Boehnhardt, B. E. A. Mueller, Wing-Huen Ip, G. LoCurto, Xin Zhou, Faith Vilas, Kevin J. Walsh, Peter H. Schultz, Y.-B. Yang, Chunhua Qi, R. Furusho, A. Zauderer, Erika L. Gibb, J. Pittichova, M. Weiler, Steven B. Charnley, Dominique Bockelée-Morvan, Gary J. Melnick, R. Vasundhara, Shigeyuki Sako, Anny Chantal Levasseur-Regourd, David J. Osip, Naruhisa Takato, Claude Arpigny, Iain Coulson, Mitchell Troy, R. Ruane, M. Kidger, Alison B. Peck, Javier Licandro, N. Moskovitz, Carl Hergenrother, Eric Pantin, David A. Neufeld, Colin Snodgrass, N. Dello Russo, Harold M. Butner, Takafumi Ootsubo, P.B. Etzel, Seiji Sugita, J. E. Thomas-Osip, Karen Magee-Sauer, Klaus-Werner Hodapp, W. Weaver, J. de León, James M. Bauer, Olivier Groussin, G. Maheswar, Tony L. Farnham, P. Rodriguez, A. Ates, F. Bensch, G. Petitas, Paul Hirst, Michael A. DiSanti, Rachel Paterno-Mahler, F. Chaffee, Patrick M. Vora, J. van Cleve, J.-M. Zucconi, Tanyu Bonev, Steve Miller, J. Ma, Martin Harwit, Z.-Y. Wu, J. A. Stüwe, Carey M. Lisse, Toshihiro Kasuga, S. Muneer, John Sarkissian, Chadwick A. Trujillo, Emanuela Pompei, Nalin H. Samarasinha, Paul D. Feldman, Qiang Li, Edith Hadamcik, Haruhiko Fujiwara, S. Yokogawa, Institute for Astronomy [Honolulu], University of Hawaii at Manoa ( UHM ), European Southern Observatory [Santiago] ( ESO ), European Southern Observatory ( ESO ), Department of Astronomy [College Park], University of Maryland [College Park], Université de Liège, Pomona College, Australian Centre for Astrobiology, University of New South Wales [Sydney] ( UNSW ), University College of London [London] ( UCL ), Universidad Metropolitana de Ciencias de la Educación ( UMCE ), Instituto de Astrofisica de Canarias ( IAC ), Jet Propulsion Laboratory ( JPL ), California Institute of Technology ( CALTECH ) -NASA, RadioAstronomisches Institut [Bonn] ( RAIUB ), Bonn Universität [Bonn], California Institute of Technology ( CALTECH ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Istituto Nazionale di Astrofisica ( INAF ), Mullard Space Science Laboratory ( MSSL ), Service d'aéronomie ( SA ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ), Atmospheric Physics Laboratory [UCL London], Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Department of Physics and Astronomy [UCL London], Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Université de Franche-Comté ( UFC ), University of Hawai‘i [Mānoa] (UHM), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), University of Maryland System-University of Maryland System, University of New South Wales [Sydney] (UNSW), University College of London [London] (UCL), Universidad Metropolitana de Ciencias de la Educación (UMCE), Instituto de Astrofisica de Canarias (IAC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Belton Space Initiatives, RadioAstronomisches Institut [Bonn] (RAIUB), Rheinische Friedrich-Wilhelms-Universität Bonn, California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, University of Toledo, Institute of Astronomy of the Bulgarian Academy of Sciences, Bulgarian Academy of Sciences (BAS), Lowell Observatory [Flagstaff], Joint Astronomy Center (JAC), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), W.M. Keck Observatory, University of Central Florida [Orlando] (UCF), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), NASA Ames Research Center (ARC), Air Force Research Laboratory (AFRL), United States Air Force (USAF), Mullard Space Science Laboratory (MSSL), University of Texas at Austin [Austin], Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Goddard Space Flight Center (GSFC), San Diego State University (SDSU), University of Maryland System, Johns Hopkins University (JHU), Western Sydney University, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Service d'aéronomie (SA), 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), Isaac Newton Group of Telescopes (ING), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Central Florida [Orlando], Western Sydney University (UWS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), and Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB)

Subjects
Cosmic Dust, Multidisciplinary, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Meteoroids, Mass ratio, 01 natural sciences, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrobiology, Photometry, Deep Impact, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Jupiter, 0103 physical sciences, Organic Chemicals, Ejecta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

著者人数: 209名, Accepted: 2005-09-01, 資料番号: SA1004082000

Published
2005
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92. Mapping the elemental composition of Ceres and Vesta: Dawn's gamma ray and neutron detector

Author

David J. Lawrence, Angioletta Coradini, Maria Teresa Capria, Donald Enemark, R. L. Williford, Thomas H. Prettyman, Carol A. Raymond, K. R. Fuller, S. A. Storms, W. C. Feldman, B. L. Barraclough, and Douglas E. Patrick

Subjects
Physics, Solar System, Planetary science, Spectrometer, Asteroid, Gamma ray, Astronomy, Asteroid belt, Neutron detection, Astrobiology, Neutron spectroscopy
Abstract

Dawn is a NASA discovery mission that will explore the main belt asteroids (1) Ceres and (4) Vesta. Ceres and Vesta are among the oldest bodies in the solar system and represent very different evolutionary paths. By studying these ancient, complementary asteroids, we will answer fundamental questions about the early solar system and planetary formation processes. The Dawn payload consists of a Framing Camera (FC), a visual and infrared mapping spectrometer (VIR), and a Gamma Ray and Neutron Detector (GRaND). The instruments provide data needed to investigate the structure, geology, mineralogy, and geochemistry of the asteroids. GRaND provides the data for the geochemistry investigation, including maps of most major elements and selected radioactive and trace elements. An updated description of the GRaND instrument is given along with the expected performance of GRaND at Vesta and Ceres. Approaches to combine data from FC, VIR and GRaND are discussed.

Published
2004
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93. C/1995 O1 Hale-Bopp: Short and Long Distance Activity From a Theoretical Model

Author

Maria Teresa Capria, Maria Cristina De Sanctis, and Angioletta Coradini

Subjects
Physics, Planetary science, Stratigraphy, Thermal, Comet, Orbit (dynamics), Astronomy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

A theoretical model of the nucleus thermal evolution and differentiation is used to simulate the evolution along the orbit of the gas and dust emissions of comet Hale-Bopp. The model was already applied to this comet (Capria et al., 2000b): At that time only the results of the observations obtained shortly after the perihelion were available. Now much more data have been published and we present more refined and complete results about the production rates of gas and dust along the orbit and the internal stratigraphy. The results of our model on long distance activity and its explanation are also presented.

Published
2002
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94. Sublimation Mechanisms of Comet Nuclei

Author

Maria Teresa Capria

Subjects
Physics, Planetary science, Comet, Theoretical models, Sublimation (phase transition), Water ice, Astrophysics, Astrobiology
Abstract

In this paper the sublimation mechanisms of parent molecules from nuclei will be reviewed from the point of view of theoretical models, and the results of models will be compared with the results of the extensive observation campaign of C/1995 O1 Hale–Bopp. The simple model of a mixture of ices in which each gas sublimates independently from the others when the right temperature has been reached is in many cases inadequate to explain the observations. Many minor volatiles can be trapped in the amorphous water ice and released in a complex way when particular ranges of temperature are reached. The presence of sublimating icy grains in the inner coma of comets, suggested many years ago, seems now to be proven, at least for Hale–Bopp. From these grains a significant amount of water and other volatiles could contribute to the total flux measured in the coma. The unprecedented coverage of Hale–Bopp’s gas production curve for such a long time and with so many instruments has offered to modellers a wonderful occasion to test and compare observation results with the predictions of sublimation models, demonstrating that current models are able to explain observed results.

Published
2002
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95. P/Wirtanen thermal evolution: effects due to the presence of an organic component in the refractory material

Author

M. I. Blecka, Angioletta Coradini, M. C. De Sanctis, and Maria Teresa Capria

Subjects
Materials science, Component (thermodynamics), CHON, Comet, Mineralogy, Astronomy and Astrophysics, Crust, Geophysics, Orders of magnitude (numbers), Silicate, chemistry.chemical_compound, thermodynamics, chemistry, Space and Planetary Science, Phase (matter), Thermal, comets
Abstract

In-situ experiments on cometary dust on board GIOTTO and VEGA missions demonstrated that in comet P/Halley's refractory component it is possible to evidentiate a refractory organic phase, the so called CHON, and a Mg-rich silicate phase. The two phases were interspersed in the individual grains. Each of these phases has different average physical properties. Laboratory experiments demonstrated that the characteristics of a crust mainly composed of silicatic particles would be different from that of a crust composed by silicatic and organic particles: thermal conductivities, for example, differ by orders of magnitude. In this paper we want to show how the simulation, in our numerical model of cometary nucleus thermal evolution, of two different dust distributions with different and independent physical properties gives us a much better modeling of the complexity of real phenomena. We attributed to one of these distributions the characteristics, taken mainly from laboratory experiments, of silicatic/organic material, and to the other one the characteristics of purely silicatic material. We applied the model to improve our simulation of comet P/Wirtanen, the target of Rosetta mission. Local temperature and evolution of the crust are different depending on which of the two distribution dominates: the maximum temperature reached by a crust with a strong organic component is lower than that reached by a purely silicatic crust.

Published
2001

96. DETECTION OF WIDESPREAD HYDRATED MATERIALS ON VESTA BY THE VIR IMAGING SPECTROMETER ON BOARD THE DAWN MISSION

Author

Jessica M. Sunshine, Maria Teresa Capria, Francesca Zambon, Andrea Longobardo, T. B. McCord, Sergio Fonte, Ernesto Palomba, David W. Mittlefehldt, J. Ph. Combe, M. C. De Sanctis, Christopher T. Russell, Carol A. Raymond, Diego Turrini, S. Marchi, Gianfranco Magni, Eleonora Ammannito, Carle M. Pieters, Alessandro Frigeri, Federico Tosi, F. Carraro, and Fabrizio Capaccioni

Subjects
Basalt, Physics, Solar System, Mineral, Space and Planetary Science, Planet, Asteroid, Imaging spectrometer, Astronomy, Terrestrial planet, Astronomy and Astrophysics, Earth (classical element), Astrobiology
Abstract

Water plays a key role in the evolution of terrestrial planets, and notably in the occurrence of Earth's oceans. However, the mechanism by which water has been incorporated into these bodies—including Earth—is still extensively debated. Here we report the detection of widespread 2.8 μm OH absorption bands on the surface of the asteroid Vesta by the VIR imaging spectrometer on board Dawn. These observations are surprising as Vesta is fully differentiated with a basaltic surface. The 2.8 μm OH absorption is distributed across Vesta's surface and shows areas enriched and depleted in hydrated materials. The uneven distribution of hydrated mineral phases is unexpected and indicates ancient processes that differ from those believed to be responsible for OH on other airless bodies, like the Moon. The origin of Vestan OH provides new insight into the delivery of hydrous materials in the main belt and may offer new scenarios on the delivery of hydrous minerals in the inner solar system, suggesting processes that may have played a role in the formation of terrestrial planets.

Published
2012
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97. The Uppsala Asteroid Data Base

Author

Maria Teresa Capria, P. Magnusson, M. Dahlgren, Anders Erikson, M. A. Barucci, Irina Belskaya, and Claes-Ingvar Lagerkvist

Subjects
Photometry (astronomy), Geography, Asteroid, Astronomy
Abstract

A collection of data and results of asteroid photometry and related observations has been made available by anonymous ftp. It contains all published asteroid lightcurve photometry, a table of reliable rotation periods, and a collection of all asteroid spin vector determinations. Here we describe the database in some detail.

Published
1994
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99. Data mining and visualization from planetary missions: the VESPA-Europlanet2020 activity

Author

Maria Teresa Capria, Marco Giardino, Andrea Longobardo, Louis Antonelli, Sergio Fonte, Angelo Zinzi, Ernesto Palomba, Europlanet Vespa Team, Paolo Giommi, Giuseppe di Persio, and Stavro Ivanovski

Subjects
010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, computer.software_genre, 01 natural sciences, Planetary missions, Visualization, Space and Planetary Science, Asteroid, 0103 physical sciences, Data mining, 010303 astronomy & astrophysics, computer, Geology, 0105 earth and related environmental sciences
Abstract

This paper presents the VESPA (Virtual European Solar and Planetary Access) activity, developed in the context of the Europlanet 2020 Horizon project, aimed at providing tools for analysis and visualization of planetary data provided by space missions. In particular, the activity is focused on minor bodies of the Solar System.The structure of the computation node, the algorithms developed for analysis of planetary surfaces and cometary comae and the tools for data visualization are presented.

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100. Pitted Terrain on Vesta and Implications for the Presence of Volatiles

Author

J. M. Sunshine, Brett W. Denevi, Frank Preusker, Federico Tosi, Maria Teresa Capria, David A. Williams, Noah E. Petro, Robert Gaskell, David T. Blewett, Simone Marchi, Debra Buczkowski, Vishnu Reddy, Fabrizio Capaccioni, M. C. De Sanctis, Andreas Nathues, W. B. Garry, Jennifer E.C. Scully, Jian-Yang Li, Christopher T. Russell, David P. O'Brien, Danielle Y. Wyrick, Paul M. Schenk, L. Le Corre, Timothy J. McCoy, Carle M. Pieters, and Carol A. Raymond

Subjects
Martian, geology, asteroid, Multidisciplinary, Planetengeodäsie, Terrain, pitted terrain, Astrobiology, Vesta, Impact crater, Asteroid, Chondrite, human activities, Geology
Abstract

Vesta to the Core Vesta is one of the largest bodies in the main asteroid belt. Unlike most other asteroids, which are fragments of once larger bodies, Vesta is thought to have survived as a protoplanet since its formation at the beginning of the solar system (see the Perspective by Binzel , published online 20 September). Based on data obtained with the Gamma Ray and Neutron Detector aboard the Dawn spacecraft, Prettyman et al. (p. 242 , published online 20 September) show that Vesta's reputed volatile-poor regolith contains substantial amounts of hydrogen delivered by carbonaceous chondrite impactors. Observations of pitted terrain on Vesta obtained by Dawn's Framing Camera and analyzed by Denevi et al. (p. 246 , published online 20 September), provide evidence for degassing of volatiles and hence the presence of hydrated materials. Finally, paleomagnetic studies by Fu et al. (p. 238 ) on a meteorite originating from Vesta suggest that magnetic fields existed on the surface of the asteroid 3.7 billion years ago, supporting the past existence of a magnetic core dynamo.

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