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Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm

dc.contributor.authorLINCOWSKI, Andrew
dc.contributor.authorMEADOWS, Victoria
dc.contributor.authorZIEBA, Sebastian
dc.contributor.authorKREIDBERG, Laura
dc.contributor.authorMORLEY, Caroline
dc.contributor.authorGILLON, Michaël
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSELSIS, Franck
dc.contributor.authorAGOL, Eric
dc.contributor.authorBOLMONT, Emeline
hal.structure.identifierCEA- Saclay [CEA]
hal.structure.identifierCentre National de la Recherche Scientifique [CNRS]
hal.structure.identifierUniversité Paris-Saclay
dc.contributor.authorDUCROT, Elsa
dc.contributor.authorHU, Renyu
dc.contributor.authorKOLL, Daniel
dc.contributor.authorLYU, Xintong
dc.contributor.authorMANDELL, Avi
dc.contributor.authorSUISSA, Gabrielle
dc.contributor.authorTAMBURO, Patrick
dc.date.issued2023-09-15
dc.identifier.issn2041-8205
dc.description.abstractEn<div><p>The first JWST observations of TRAPPIST-1 c showed a secondary eclipse depth of 421±94 ppm at 15 µm, which is consistent with a bare rock surface or a thin, O 2 -dominated, low CO 2 atmosphere (Zieba et al. 2023).</p><p>Here, we further explore potential atmospheres for TRAPPIST-1 c by comparing the observed secondary eclipse depth to synthetic spectra of a broader range of plausible environments. To self-consistently incorporate the impact of photochemistry and atmospheric composition on atmospheric thermal structure and predicted eclipse depth, we use a two-column climate model coupled to a photochemical model, and simulate O 2 -dominated, Venus-like, and steam atmospheres. We find that a broader suite of plausible atmospheric compositions are also consistent with the data. For lower pressure atmospheres (0.1 bar), our O 2 -CO 2 atmospheres produce eclipse depths within 1σ of the data, consistent with the modeling results of Zieba et al. (2023). However, for higherpressure atmospheres, our models produce different temperature-pressure profiles and are less pessimistic, with 1-10 bar O 2 , 100 ppm CO 2 models within 2.0-2.2σ of the measured secondary eclipse depth, and up to 0.5% CO 2 within 2.9σ. Venus-like atmospheres are still unlikely. For thin O 2 atmospheres of 0.1 bar with a low abundance of CO 2 (∼100 ppm), up to 10% water vapor can be present and still provide an eclipse depth within 1σ of the data. We compared the TRAPPIST-1 c data to modeled steam atmospheres of ≤ 3 bar, which are 1.7-1.8σ from the data and not conclusively ruled out. More data will be required to discriminate between possible atmospheres, or to more definitively support the bare rock hypothesis.</p></div>
dc.language.isoen
dc.publisherBristol : IOP Publishing
dc.title.enPotential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
dc.typeArticle de revue
dc.identifier.doi10.3847/2041-8213/acee02
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv2308.05899
bordeaux.journalThe Astrophysical journal letters
bordeaux.pageL7
bordeaux.volume955
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-04790353
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04790353v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=The%20Astrophysical%20journal%20letters&amp;rft.date=2023-09-15&amp;rft.volume=955&amp;rft.issue=1&amp;rft.spage=L7&amp;rft.epage=L7&amp;rft.eissn=2041-8205&amp;rft.issn=2041-8205&amp;rft.au=LINCOWSKI,%20Andrew&amp;MEADOWS,%20Victoria&amp;ZIEBA,%20Sebastian&amp;KREIDBERG,%20Laura&amp;MORLEY,%20Caroline&amp;rft.genre=article


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