Mostrar el registro sencillo del ítem

A chemical model for the atmosphere of hot Jupiters

hal.structure.identifierSSE 2012
dc.contributor.authorVENOT, O.
hal.structure.identifierSSE 2012
dc.contributor.authorHÉBRARD, Eric
hal.structure.identifierSSE 2012
dc.contributor.authorAGÚNDEZ, M.
hal.structure.identifierSSE 2012
dc.contributor.authorDOBRIJEVIC, M.
hal.structure.identifierSSE 2012
dc.contributor.authorSELSIS, Franck
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERSANT, F.
hal.structure.identifierDept of Physics
dc.contributor.authorIRO, Nicolas
hal.structure.identifierLaboratoire Réactions et Génie des Procédés [LRGP]
dc.contributor.authorBOUNACEUR, Roda
dc.date.created2012-08-02
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnOur purpose is to release a chemical network, and the associated rate coefficients, developed for the temperature and pressure range relevant to hot Jupiters atmospheres. Using this network, we study the vertical atmospheric composition of the two hot Jupiters (HD209458b, HD189733b) with a model that includes photolyses and vertical mixing and we produce synthetic spectra. The chemical scheme is derived from applied combustion models that have been methodically validated over a range of temperatures and pressures typical of the atmospheric layers influencing the observations of hot Jupiters. We compare the predictions obtained from this scheme with equilibrium calculations, with different schemes available in the literature that contain N-bearing species and with previously published photochemical models. Compared to other chemical schemes that were not subjected to the same systematic validation, we find significant differences whenever non-equilibrium processes take place. The deviations from the equilibrium, and thus the sensitivity to the network, are more important for HD189733b, as we assume a cooler atmosphere than for HD209458b. We found that the abundances of NH3 and HCN can vary by two orders of magnitude depending on the network, demonstrating the importance of comprehensive experimental validation. A spectral feature of NH3 at 10.5$\mu$m is sensitive to these abundance variations and thus to the chemical scheme. Due to the influence of the kinetics, we recommend the use of a validated scheme to model the chemistry of exoplanet atmospheres. Our network is robust for temperatures within 300-2500K and pressures from 10mbar up to a few hundreds of bars, for species made of C,H,O,N. It is validated for species up to 2 carbon atoms and for the main nitrogen species.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enastrochemistry
dc.subject.enplanets and satellites: atmospheres
dc.subject.enplanets and satellites: individual: HD 209458b
dc.subject.enplanets and satellites: individual: HD 189733b
dc.subject.enplanetary systems
dc.title.enA chemical model for the atmosphere of hot Jupiters
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201219310
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1208.0560
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A43, 19 pp
bordeaux.volume546
bordeaux.peerReviewedoui
hal.identifierhal-00764601
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00764601v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2012&rft.volume=546&rft.spage=id.A43,%2019%20pp&rft.epage=id.A43,%2019%20pp&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=VENOT,%20O.&H%C3%89BRARD,%20Eric&AG%C3%9ANDEZ,%20M.&DOBRIJEVIC,%20M.&SELSIS,%20Franck&rft.genre=article


Archivos en el ítem

ArchivosTamañoFormatoVer

No hay archivos asociados a este ítem.

Este ítem aparece en la(s) siguiente(s) colección(ones)

Mostrar el registro sencillo del ítem