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Virtis: An Imaging Spectrometer for the Rosetta Mission

Coradini, A. and Capaccioni, F. and Drossart, P. and Arnold, G. and Ammannito, E. and Angrilli, F. and Barucci, A. and Belllucci, J. and Benkhoff, J. and Bianchini, G. and Bibring, J.P. and Blecka, M. and Bockelee-Morvan, D. and Capria, M.T. and Carlson, R. and Carsenty, U. and Cerroni, P. and Colangeli, L. and Combes, M. and Combi, M. and Crovisier, J. and Desanctis, M.C. and Encrenaz, E.T. and Erard, S. and Federico, C. and Filacchione, G. and Fink, U. and Fonti, S. and Formisano, V. and Ip, W.H. and Jaumann, R. and Kührt, E. and Langevin, Y. and Magni, G. and Mccord, T. and Mennella, V. and Mottola, S. and Neukum, G. and Palumbo, P. and Piccioni, G. and Rauer, H. and Saggin, B. and Schmitt, B. and Tiphene, D. and Tozzi, G. (2007) Virtis: An Imaging Spectrometer for the Rosetta Mission. Space Science Reviews, 128 (1), pp. 529-559. Springer. doi: 10.1007/s11214-006-9127-5. ISSN 0038-6308.

Full text not available from this repository.

Official URL: http://www.springerlink.com/content/w471050wg15w2q06/

Abstract

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.

Item URL in elib:https://elib.dlr.de/47577/
Document Type:Article
Additional Information:bisher nur Online-Veroeffentlichung, Druck folgt noch
Title:Virtis: An Imaging Spectrometer for the Rosetta Mission
Authors:
AuthorsInstitution or Email of AuthorsAuthor's ORCID iDORCID Put Code
Coradini, A.INAF, Istituto di Fisica Dello Spazio Interplanetario, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Capaccioni, F.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Drossart, P.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Arnold, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ammannito, E.INAF, Istituto di Fisica Dello Spazio Interplanetario, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Angrilli, F.Dipartimento di Ingneria Meccanica, Università di PadovaUNSPECIFIEDUNSPECIFIED
Barucci, A.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Belllucci, J.INAF, Istituto di Fisica Dello Spazio Interplanetario, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Benkhoff, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Bianchini, G.Dipartimento di Ingneria Meccanica, Università di PadovaUNSPECIFIEDUNSPECIFIED
Bibring, J.P.Institut d'Astrophysique Spatial CNRS, Orsay, FranceUNSPECIFIEDUNSPECIFIED
Blecka, M.Polish Academi of Sciences, Warsaw, PolandUNSPECIFIEDUNSPECIFIED
Bockelee-Morvan, D.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Capria, M.T.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Carlson, R.NASA JPL, Pasadena, USAUNSPECIFIEDUNSPECIFIED
Carsenty, U.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Cerroni, P.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Colangeli, L.Osservatorio di Capodimonte, Napoli, ItalyUNSPECIFIEDUNSPECIFIED
Combes, M.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Combi, M.Space Physics Research Laboratory, The University of Michigan, Ann Arbor, USAUNSPECIFIEDUNSPECIFIED
Crovisier, J.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Desanctis, M.C.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Encrenaz, E.T.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Erard, S.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Federico, C.Università di Perugia, ItalyUNSPECIFIEDUNSPECIFIED
Filacchione, G.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Fink, U.Lunar Planetary Laboratory, Univarsity of Arizona, Tucson, USAUNSPECIFIEDUNSPECIFIED
Fonti, S.Dipartimento di Fisica, Università di Lecce, ItalyUNSPECIFIEDUNSPECIFIED
Formisano, V.INAF, Istituto di Fisica Dello Spazio Interplanetario, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Ip, W.H.MPI, Katlenburg, GermanyUNSPECIFIEDUNSPECIFIED
Jaumann, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kührt, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Langevin, Y.Institut d'Astrophysique Spatial CNRS, Orsay, FranceUNSPECIFIEDUNSPECIFIED
Magni, G.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Mccord, T.Department of Earth and Space Science, University of Washington, Seattle, USAUNSPECIFIEDUNSPECIFIED
Mennella, V.Osservatorio di Capodimonte, Napoli, ItalyUNSPECIFIEDUNSPECIFIED
Mottola, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Neukum, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Palumbo, P.Osservatorio di Capodimonte, Napoli, ItalyUNSPECIFIEDUNSPECIFIED
Piccioni, G.INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Roma, ItalyUNSPECIFIEDUNSPECIFIED
Rauer, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Saggin, B.Dipartimento di Ingneria Meccanica, Università di PadovaUNSPECIFIEDUNSPECIFIED
Schmitt, B.Laboratoire de Glaciologie et Geophysique de l'Environment, Grenoble, FranceUNSPECIFIEDUNSPECIFIED
Tiphene, D.LESIA Observatoire de Paris, Meudon, FranceUNSPECIFIEDUNSPECIFIED
Tozzi, G.Osservatorio Astrofisico di Arcetri, Firenze, ItalyUNSPECIFIEDUNSPECIFIED
Date:22 February 2007
Journal or Publication Title:Space Science Reviews
Open Access:No
Gold Open Access:No
In SCOPUS:Yes
In ISI Web of Science:Yes
Volume:128
DOI:10.1007/s11214-006-9127-5
Page Range:pp. 529-559
Publisher:Springer
ISSN:0038-6308
Status:Published
Keywords:Comets, spectroscopy, space mission
HGF - Research field:Aeronautics, Space and Transport (old)
HGF - Program:Space (old)
HGF - Program Themes:W EW - Erforschung des Weltraums
DLR - Research area:Space
DLR - Program:W EW - Erforschung des Weltraums
DLR - Research theme (Project):W - Projekt ROSETTA Instrumente (old)
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research
Institute of Planetary Research > Extrasolar Planets and Atmospheres
Institute of Planetary Research > Planetary Geology
Institute of Planetary Research > Asteroids and Comets
Deposited By: Carsenty, Dr.rer.nat. Uri
Deposited On:14 Mar 2007
Last Modified:07 Aug 2017 10:54

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