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Water Condensation Zones around Main Sequence Stars

hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
hal.structure.identifierInstitut Pierre-Simon-Laplace [IPSL (FR_636)]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorTURBET, Martin
dc.contributor.authorFAUCHEZ, Thomas
dc.contributor.authorLECONTE, Jeremy
dc.contributor.authorBOLMONT, Emeline
dc.contributor.authorCHAVEROT, Guillaume
dc.contributor.authorFORGET, Francois
dc.contributor.authorMILLOUR, Ehouarn
dc.contributor.authorSELSIS, Franck
dc.contributor.authorCHARNAY, Benjamin
dc.contributor.authorDUCROT, Elsa
dc.contributor.authorGILLON, Michaël
dc.contributor.authorMAUREL, Alice
dc.contributor.authorVILLANUEVA, Geronimo
dc.date.issued2023
dc.description.abstractEnUnderstanding the set of conditions that allow rocky planets to have liquid water on their surface -- in the form of lakes, seas or oceans -- is a major scientific step to determine the fraction of planets potentially suitable for the emergence and development of life as we know it on Earth. This effort is also necessary to define and refine the so-called "Habitable Zone" (HZ) in order to guide the search for exoplanets likely to harbor remotely detectable life forms. Until now, most numerical climate studies on this topic have focused on the conditions necessary to maintain oceans, but not to form them in the first place. Here we use the three-dimensional Generic Planetary Climate Model (PCM), historically known as the LMD Generic Global Climate Model (GCM), to simulate water-dominated planetary atmospheres around different types of Main-Sequence stars. The simulations are designed to reproduce the conditions of early ocean formation on rocky planets due to the condensation of the primordial water reservoir at the end of the magma ocean phase. We show that the incoming stellar radiation (ISR) required to form oceans by condensation is always drastically lower than that required to vaporize oceans. We introduce a Water Condensation Limit, which lies at significantly lower ISR than the inner edge of the HZ calculated with three-dimensional numerical climate simulations. This difference is due to a behavior change of water clouds, from low-altitude dayside convective clouds to high-altitude nightside stratospheric clouds. Finally, we calculated transit spectra, emission spectra and thermal phase curves of TRAPPIST-1b, c and d with H2O-rich atmospheres, and compared them to CO2 atmospheres and bare rock simulations. We show using these observables that JWST has the capability to probe steam atmospheres on low-mass planets, and could possibly test the existence of nightside water clouds.
dc.language.isoen
dc.subject.enEarth and Planetary Astrophysics (astro-ph.EP)
dc.subject.enAtmospheric and Oceanic Physics (physics.ao-ph)
dc.subject.enGeophysics (physics.geo-ph)
dc.subject.enFOS: Physical sciences
dc.title.enWater Condensation Zones around Main Sequence Stars
dc.typeDocument de travail - Pré-publication
dc.identifier.doi10.48550/arXiv.2308.15110
dc.subject.halPlanète et Univers [physics]
dc.identifier.arxiv2308.15110
hal.identifierhal-04263315
hal.version1
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04263315v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.date=2023&rft.au=TURBET,%20Martin&FAUCHEZ,%20Thomas&LECONTE,%20Jeremy&BOLMONT,%20Emeline&CHAVEROT,%20Guillaume&rft.genre=preprint


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