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hal.structure.identifierECLIPSE 2015
dc.contributor.authorVON PARIS, P.
hal.structure.identifierECLIPSE 2015
dc.contributor.authorSELSIS, Franck
dc.contributor.authorGODOLT, M.,
hal.structure.identifierNottingham Transportation Engineering Centre
dc.contributor.authorGRENFELL, J. L.,
dc.contributor.authorSTRACKE, B.,
hal.structure.identifierDLR Institut für Planetenforschung
dc.contributor.authorRAUER, H.,
dc.date.issued2015
dc.identifier.issn0019-1035
dc.description.abstractEnOzone is an important radiative trace gas in the Earth's atmosphere. The presence of ozone can significantly influence the thermal structure of an atmosphere, and by this e.g. cloud formation. Photochemical studies suggest that ozone can form in carbon dioxide-rich atmospheres. We investigate the effect of ozone on the temperature structure of simulated early Martian atmospheres. With a 1D radiative-convective model, we calculate temperature-pressure profiles for a 1 bar carbon dioxide atmosphere. Ozone profiles are fixed, parameterized profiles. We vary the location of the ozone layer maximum and the concentration at this maximum. The maximum is placed at different pressure levels in the upper and middle atmosphere (1-10 mbar). Results suggest that the impact of ozone on surface temperatures is relatively small. However, the planetary albedo significantly decreases at large ozone concentrations. Throughout the middle and upper atmospheres, temperatures increase upon introducing ozone due to strong UV absorption. This heating of the middle atmosphere strongly reduces the zone of carbon dioxide condensation, hence the potential formation of carbon dioxide clouds. For high ozone concentrations, the formation of carbon dioxide clouds is inhibited in the entire atmosphere. In addition, due to the heating of the middle atmosphere, the cold trap is located at increasingly higher pressures when increasing ozone. This leads to wetter stratospheres hence might increase water loss rates on early Mars. However, increased stratospheric H2O would lead to more HOx, which could efficiently destroy ozone. This result emphasizes the need for consistent climate-chemistry calculations to assess the feedback between temperature structure, water content and ozone chemistry. Furthermore, convection is inhibited at high ozone amounts, leading to a stably stratified atmosphere.
dc.language.isoen
dc.publisherElsevier
dc.title.enEffect of O3 on the atmospheric temperature structure of early Mars
dc.typeArticle de revue
dc.identifier.doi10.1016/j.icarus.2015.05.028
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.identifier.arxiv1505.07713
bordeaux.journalIcarus
bordeaux.page406-416
bordeaux.volume257
bordeaux.peerReviewedoui
hal.identifierhal-01158387
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01158387v1
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