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Composition of Ices in Low-Mass Extrasolar Planets

hal.structure.identifierUnivers, Théorie, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) [UTINAM]
dc.contributor.authorMARBOEUF, U.
hal.structure.identifierUnivers, Théorie, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) [UTINAM]
dc.contributor.authorMOUSIS, O.
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
hal.structure.identifierLaboratoire d'Astrophysique de Grenoble [LAOG]
dc.contributor.authorEHRENREICH, D.
hal.structure.identifierUnivers, Théorie, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) [UTINAM]
hal.structure.identifierAstronomische Rechen-Institut [Heidelberg] [ARI]
dc.contributor.authorALIBERT, Yann
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
hal.structure.identifierAstronomische Rechen-Institut [Heidelberg] [ARI]
dc.contributor.authorCASSAN, A.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierDepartment of Physics
hal.structure.identifierThe Ohio State University [Columbus] [OSU]
hal.structure.identifierDepartment of Physics [OSU]
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorBEAULIEU, J.-P.
dc.date.created2008
dc.date.issued2008
dc.identifier.issn0004-637X
dc.description.abstractEnWe study the formation conditions of icy planetesimals in protoplanetary disks in order to determine the composition of ices in small and cold extrasolar planets. Assuming that ices are formed from hydrates, clathrates, and pure condensates, we calculate their mass fractions with respect to the total quantity of ices included in planetesimals, for a grid of disk models. We find that the composition of ices weakly depends on the adopted disk thermodynamic conditions, and is rather influenced by the initial composition of the gas phase. The use of a plausible range of molecular abundance ratios and the variation of the relative elemental carbon over oxygen ratio in the gas phase of protoplanetary disks allow us to apply our model to a wide range of planetary systems. Our results can thus be used to constrain the icy/volatile phase composition of cold planets evidenced by microlensing surveys, hypothetical ocean planets, and carbon planets, which could be detected by COROT or Kepler.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enStars: Planetary Systems
dc.subject.enStars: Planetary Systems: Formation
dc.title.enComposition of Ices in Low-Mass Extrasolar Planets
dc.typeArticle de revue
dc.identifier.doi10.1086/588777
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv0804.0406
bordeaux.journalThe Astrophysical Journal
bordeaux.page1624-1630
bordeaux.volume681
bordeaux.peerReviewedoui
hal.identifierhal-00270957
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00270957v1
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