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hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorCAVALIÉ, Thibault
hal.structure.identifierCatholic University of Leuven = Katholieke Universiteit Leuven [KU Leuven]
dc.contributor.authorVENOT, Olivia
hal.structure.identifierECLIPSE 2017
dc.contributor.authorSELSIS, Franck
hal.structure.identifierECLIPSE 2017
dc.contributor.authorHERSANT, F.
hal.structure.identifierMax-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research [MPS]
dc.contributor.authorHARTOGH, Paul
hal.structure.identifierECLIPSE 2017
dc.contributor.authorLECONTE, J.
dc.date.issued2017-03
dc.identifier.issn0019-1035
dc.description.abstractEnThermochemical models have been used in the past to constrain the deep oxygen abundance in the gas and ice giant planets from tropospheric CO spectroscopic measurements. Knowing the oxygen abundance of these planets is a key to better understand their formation. These models have widely used dry and/or moist adiabats to extrapolate temperatures from the measured values in the upper troposphere down to the level where the thermochemical equilibrium between H$_2$O and CO is established. The mean molecular mass gradient produced by the condensation of H$_2$O stabilizes the atmosphere against convection and results in a vertical thermal profile and H$_2$O distribution that departs significantly from previous estimates. We revisit O/H estimates using an atmospheric structure that accounts for the inhibition of the convection by condensation. We use a thermochemical network and the latest observations of CO in Uranus and Neptune to calculate the internal oxygen enrichment required to satisfy both these new estimates of the thermal profile and the observations. We also present the current limitations of such modeling.
dc.language.isoen
dc.publisherElsevier
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.title.enThermochemistry and vertical mixing in the tropospheres of Uranus and Neptune: How convection inhibition can affect the derivation of deep oxygen abundances
dc.typeArticle de revue
dc.identifier.doi10.1016/j.icarus.2017.03.015
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1703.04358
bordeaux.journalIcarus
bordeaux.page1-16
bordeaux.volume291
bordeaux.peerReviewedoui
hal.identifierhal-01489193
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01489193v1
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