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Exploring the Internal Structures of hot Jupiters using the GCM DYNAMICO: Deep, Hot, Adiabats as a Possible Solution to the Radius Inflation Problem

dc.contributor.authorSAINSBURY-MARTINEZ, Felix
dc.contributor.authorWANG, Pascal
dc.contributor.authorFROMANG, Sebastian
hal.structure.identifierMaison de la Simulation [MDLS]
dc.contributor.authorTREMBLIN, Pascal
hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
dc.contributor.authorDUBOS, Thomas
hal.structure.identifierLaboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] [LSCE]
dc.contributor.authorMEURDESOIF, Yann
hal.structure.identifierECLIPSE 2019
dc.contributor.authorLECONTE, J.
hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
dc.contributor.authorSPIGA, Aymeric
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorBARAFFE, Isabelle
hal.structure.identifierSchool of Physics and Astronomy [Exeter]
dc.contributor.authorMAYNE, Nathan
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorDEBRAS, Florian
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorCHABRIER, Gilles
dc.contributor.authorDRUMMOND, Ben
dc.date.issued2019
dc.identifier.issn0002-7537
dc.description.abstractEnThe anomalously large radii of highly irradiated exoplanets have long remained a mystery to the Exoplanetary community, with many different solutions suggested and tested. These solutions have included tidal heating of the atmosphere, or ohmic heating from a strong magnetic field. Another solution was also suggested by Tremblin et Al. (2017): The inflated radii of highly irradiated exoplanets can be explained by the advection of potential temperature, via mass and longitudinal momentum conservation, leads to the deep atmosphere attaching to a hotter adiabat than would be suggested by 1D models, thus implying an inflated radius. In that paper this mechanism was tested using 2D steady-state models, and successfully reproduced an inflated HD209458b scenario. Here we extend this work to both the time-dependent and 3D regimes using the GCM Dynamico (Itself developed as a new dynamical core for LMD-Z, and verified against Hot Jupiter benchmarks as part of this work), exploring the evolution of the deep P-T profile, and the stability of a deep adiabat as the steady state solution. As a result of these calculations we confirm that a deep, hot, adiabat is both the target of long term evolution of the deep atmosphere, and is stable against typical forcing expected at deep pressures — we also note that this deep adiabat takes a very significant time to form from an isothermal initial condition (hence why it has not previously been seen in GCM simulations beyond a kink in the deep profile), and suggest that future GCM models should use an adiabatic profile to initialise the deep atmosphere. Taken as a whole, our results confirm the theory of Tremblin et Al. (2017): the inflated radii of highly irradiated exoplanets can be explained by connecting the atmosphere with a deep, hot, internal adiabat.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.title.enExploring the Internal Structures of hot Jupiters using the GCM DYNAMICO: Deep, Hot, Adiabats as a Possible Solution to the Radius Inflation Problem
dc.typeArticle de revue
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
bordeaux.journalBulletin of the American Astronomical Society
bordeaux.volume51
bordeaux.issue6
bordeaux.peerReviewedoui
hal.identifierhal-02298731
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02298731v1
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