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dc.contributor.authorJuncher, Diana
dc.contributor.authorJørgensen, Uffe G.
dc.contributor.authorHelling, Christiane
dc.date.accessioned2018-01-04T12:30:11Z
dc.date.available2018-01-04T12:30:11Z
dc.date.issued2017-12
dc.identifier.citationJuncher , D , Jørgensen , U G & Helling , C 2017 , ' Self-consistent atmosphere modeling with cloud formation for low-mass stars and exoplanets ' , Astronomy and Astrophysics , vol. 608 , A70 . https://doi.org/10.1051/0004-6361/201629977en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 251875278
dc.identifier.otherPURE UUID: 5a26951f-d478-4046-bd02-fcb6b50b3d1d
dc.identifier.otherScopus: 85038209286
dc.identifier.otherWOS: 000417620200004
dc.identifier.urihttp://hdl.handle.net/10023/12426
dc.descriptionChH highlight financial support of the European Community under the FP7 by the ERC starting grant 257431.en
dc.description.abstractContext.  Low-mass stars and extrasolar planets have ultra-cool atmospheres where a rich chemistry occurs and clouds form. The increasing amount of spectroscopic observations for extrasolar planets requires self-consistent model atmosphere simulations to consistently include the formation processes that determine cloud formation and their feedback onto the atmosphere. Aims.  Our aim is to complement the Marcs model atmosphere suit with simulations applicable to low-mass stars and exoplanets in preparation of E-ELT, JWST, PLATO and other upcoming facilities. Methods.  The Marcs code calculates stellar atmosphere models, providing self-consistent solutions of the radiative transfer and the atmospheric structure and chemistry. We combine Marcs with a kinetic model that describes cloud formation in ultra-cool atmospheres (seed formation, growth/evaporation, gravitational settling, convective mixing, element depletion). Results. We present a small grid of self-consistently calculated atmosphere models for Teff = 2000-3000 K with solar initial abundances and log(g) = 4:5. Cloud formation in stellar and sub-stellar atmospheres appears for Teff < 2700 K and has a significant effect on the structure and the spectrum of the atmosphere for Teff < 2400 K. We have compared the synthetic spectra of our models with observed spectra and found that they fit the spectra of mid-To late-Type M-dwarfs and early-Type L-dwarfs well. The geometrical extension of the atmospheres (at τ = 1) changes with wavelength resulting in a flux variation of ∼ 10%. This translates into a change in geometrical extension of the atmosphere of about 50 km, which is the quantitative basis for exoplanetary transit spectroscopy.We also test Drift-Marcs for an example exoplanet and demonstrate that our simulations reproduce the Spitzer observations for WASP-19b rather well for Teff = 2600 K, log(g) = 3:2 and solar abundances. Our model points at an exoplanet with a deep cloud-free atmosphere with a substantial day-night energy transport and no temperature inversion.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysicsen
dc.rights© ESO, 2017. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201629977en
dc.subjectAstrochemistryen
dc.subjectMethods: numericalen
dc.subjectRadiative transferen
dc.subjectStars: atmospheresen
dc.subjectStars: low-mass, brown dwarfsen
dc.subjectQB Astronomyen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectNDASen
dc.subject.lccQBen
dc.titleSelf-consistent atmosphere modeling with cloud formation for low-mass stars and exoplanetsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201629977
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1708.06976en
dc.identifier.grantnumber257431 257431en


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