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dc.contributor.authorWoitke, P.
dc.contributor.authorHerbort, O.
dc.contributor.authorHelling, Ch
dc.contributor.authorStüeken, E.
dc.contributor.authorDominik, M.
dc.contributor.authorBarth, P.
dc.contributor.authorSamra, D.
dc.date.accessioned2020-11-06T17:30:02Z
dc.date.available2020-11-06T17:30:02Z
dc.date.issued2020-10-17
dc.identifier.citationWoitke , P , Herbort , O , Helling , C , Stüeken , E , Dominik , M , Barth , P & Samra , D 2020 , ' Coexistence of CH 4 , CO 2 and H 2 O in exoplanet atmospheres ' , Astronomy & Astrophysics , vol. Forthcoming . https://doi.org/10.1051/0004-6361/202038870en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 271085660
dc.identifier.otherPURE UUID: 3f9be364-d2d0-4b51-bb1b-c8c6b1b057ec
dc.identifier.otherArXiv: http://arxiv.org/abs/2010.12241v1
dc.identifier.otherScopus: 85100698785
dc.identifier.otherWOS: 000617516200001
dc.identifier.urihttp://hdl.handle.net/10023/20921
dc.descriptionP.W. and Ch.H. acknowledge funding from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). O.H. acknowledges the PhD stipend form the University of St Andrews’ Centre for Exoplanet Science. P.B. acknowledges support from the St Leonards interdisciplinary scholarship.en
dc.description.abstractWe propose a classification of exoplanet atmospheres based on their H, C, O, N element abundances below about 600 K. Chemical equilibrium models were run for all combinations of H, C, N, O abundances, and three types of solutions were found, which are robust against variations of temperature, pressure and nitrogen abundance. Type A atmospheres contain H2O, CH4, NH3 and either H2 or N2, but only traces of CO2 and O2. Type B atmospheres contain O2, H2O, CO2 and N2, but only traces of CH4, NH3 and H2. Type C atmospheres contain H2O, CO2, CH4 and N2, but only traces of NH3, H2 and O2. Other molecules are only present in ppb or ppm concentrations in chemical equilibrium, depending on temperature. Type C atmospheres are not found in the solar system, where atmospheres are generally cold enough for water to condense, but exoplanets may well host such atmospheres. Our models show that graphite (soot) clouds can occur in type C atmospheres in addition to water clouds, which can occur in all types of atmospheres. Full equilibrium condensation models show that the outgassing from warm rock can naturally provide type C atmospheres. We conclude that type C atmospheres, if they exist, would lead to false positive detections of biosignatures in exoplanets when considering the coexistence of CH4 and CO2, and suggest other, more robust non-equilibrium markers.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © 2020 ESO. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://www.aanda.org/.en
dc.subjectPlanets and satellites: atmospheresen
dc.subjectPlanets and satellites: compositionen
dc.subjectAstrochemistryen
dc.subjectQC Physicsen
dc.subjectQD Chemistryen
dc.subject3rd-DASen
dc.subject.lccQCen
dc.subject.lccQDen
dc.titleCoexistence of CH4, CO2 and H2O in exoplanet atmospheresen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.contributor.institutionUniversity of St Andrews.School of Earth & Environmental Sciencesen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202038870
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2010.12241en


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