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Simulations of Water Vapor and Clouds on Rapidly Rotating and Tidally Locked Planets: A 3D Model Intercomparison

hal.structure.identifierBeihang University [BUAA]
dc.contributor.authorYANG, Jun
hal.structure.identifierECLIPSE 2019
dc.contributor.authorLECONTE, J.
hal.structure.identifierBritish Antarctic Survey [BAS]
dc.contributor.authorWOLF, Eric
hal.structure.identifierMcGill University = Université McGill [Montréal, Canada]
dc.contributor.authorMERLIS, Timothy
dc.contributor.authorKOLL, Daniel
hal.structure.identifierLaboratoire de Météorologie Dynamique (UMR 8539) [LMD]
dc.contributor.authorFORGET, François
dc.contributor.authorABBOT, Dorian
dc.date.issued2019-04-10
dc.identifier.issn0004-637X
dc.description.abstractEnRobustly modeling the inner edge of the habitable zone is essential for determining the most promising potentially habitable exoplanets for atmospheric characterization. Global climate models (GCMs) have become the standard tool for calculating this boundary, but divergent results have emerged among the various GCMs. In this study, we perform an intercomparison of standard GCMs used in the field on a rapidly rotating planet receiving a G-star spectral energy distribution and on a tidally locked planet receiving an M-star spectral energy distribution. Experiments both with and without clouds are examined. We find relatively small difference (within 8 K) in global-mean surface temperature simulation among the models in the G-star case with clouds. In contrast, the global-mean surface temperature simulation in the M-star case is highly divergent (20–30 K). Moreover, even differences in the simulated surface temperature when clouds are turned off are significant. These differences are caused by differences in cloud simulation and/or radiative transfer, as well as complex interactions between atmospheric dynamics and these two processes. For example we find that an increase in atmospheric absorption of shortwave radiation can lead to higher relative humidity at high altitudes globally and, therefore, a significant decrease in planetary radiation emitted to space. This study emphasizes the importance of basing conclusions about planetary climate on simulations from a variety of GCMs and motivates the eventual comparison of GCM results with terrestrial exoplanet observations to improve their performance.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.title.enSimulations of Water Vapor and Clouds on Rapidly Rotating and Tidally Locked Planets: A 3D Model Intercomparison
dc.typeArticle de revue
dc.identifier.doi10.3847/1538-4357/ab09f1
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1912.11329
bordeaux.journalThe Astrophysical Journal
bordeaux.page46
bordeaux.volume875
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-02101711
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02101711v1
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