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Origin of volatiles in the Main Belt

hal.structure.identifierLaboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) [LAOB]
dc.contributor.authorMOUSIS, Olivier
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorALIBERT, Yann
hal.structure.identifierInstitut de Mécanique Céleste et de Calcul des Ephémérides [IMCCE]
dc.contributor.authorHESTROFFER, D.
hal.structure.identifierLaboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) [LAOB]
dc.contributor.authorMARBOEUF, Ulysse
hal.structure.identifierLaboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) [LAOB]
hal.structure.identifierCentre de Biochimie Structurale [Montpellier] [CBS]
hal.structure.identifierReproduction et développement des plantes [RDP]
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorDUMAS, Christophe
hal.structure.identifierLaboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) [LAOB]
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorCARRY, Benoit
dc.contributor.authorHORNER, Jonathan
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSELSIS, Franck
dc.date.issued2008
dc.identifier.issn0035-8711
dc.description.abstractEnWe propose a scenario for the formation of the Main Belt in which asteroids incorporated icy particles formed in the outer Solar Nebula. We calculate the composition of icy planetesimals formed beyond a heliocentric distance of 5 AU in the nebula by assuming that the abundances of all elements, in particular that of oxygen, are solar. As a result, we show that ices formed in the outer Solar Nebula are composed of a mix of clathrate hydrates, hydrates formed above 50 K and pure condensates produced at lower temperatures. We then consider the inward migration of solids initially produced in the outer Solar Nebula and show that a significant fraction may have drifted to the current position of the Main Belt without encountering temperature and pressure conditions high enough to vaporize the ices they contain. We propose that, through the detection and identification of initially buried ices revealed by recent impacts on the surfaces of asteroids, it could be possible to infer the thermodynamic conditions that were present within the Solar Nebula during the accretion of these bodies, and during the inward migration of icy planetesimals. We also investigate the potential influence that the incorporation of ices in asteroids may have on their porosities and densities. In particular, we show how the presence of ices reduces the value of the bulk density of a given body, and consequently modifies its macro-porosity from that which would be expected from a given taxonomic type.
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.subject.enasteroids
dc.subject.enminor planets
dc.subject.ensolar system: formation
dc.subject.enasteroids.
dc.title.enOrigin of volatiles in the Main Belt
dc.typeArticle de revue
dc.identifier.doi10.1111/j.1365-2966.2007.12653.x
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv0710.5179
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page1269-1280
bordeaux.volume383
bordeaux.issue3
bordeaux.peerReviewedoui
hal.identifierhal-00265967
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00265967v1
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