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dc.contributor.authorHelling, Christiane
dc.contributor.authorCasewell, Sarah
dc.date.accessioned2015-11-16T00:11:32Z
dc.date.available2015-11-16T00:11:32Z
dc.date.issued2014
dc.identifier.citationHelling , C & Casewell , S 2014 , ' Atmospheres of brown dwarfs ' , Astronomy and Astrophysics Review , vol. 22 , 80 . https://doi.org/10.1007/s00159-014-0080-0en
dc.identifier.issn0935-4956
dc.identifier.otherPURE: 156879888
dc.identifier.otherPURE UUID: 52e8e302-3538-41b4-9720-6a355870a58c
dc.identifier.otherArXiv: http://arxiv.org/abs/1410.6029v1
dc.identifier.otherScopus: 84919919061
dc.identifier.otherWOS: 000348389300001
dc.identifier.urihttp://hdl.handle.net/10023/7785
dc.descriptionChH highlights financial support of the European Community under the FP7 by an ERC starting grant. SLC acknowledges financial support of University of Leicesteren
dc.description.abstractBrown Dwarfs are the coolest class of stellar objects known to date. Our present perception is that Brown Dwarfs follow the principles of star formation, and that Brown Dwarfs share many characteristics with planets. Being the darkest and lowest mass stars known makes Brown Dwarfs also the coolest stars known. This has profound implication for their spectral fingerprints. Brown Dwarfs cover a range of effective temperatures which cause brown dwarfs atmospheres to be a sequence that gradually changes from a M-dwarf-like spectrum into a planet-like spectrum. This further implies that below an effective temperature of ≲ 2800K, clouds form already in atmospheres of objects marking the boundary between M-Dwarfs and brown dwarfs. Recent developments have sparked the interest in plasma processes in such very cool atmospheres: sporadic and quiescent radio emission has been observed in combination with decaying Xray-activity indicators across the fully convective boundary.
dc.format.extent45
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics Reviewen
dc.rights© 2014, Springer. This work is 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 publication is available at Springer via http://dx.doi.org/10.1007/s00159-014-0080-0en
dc.subjectStars: brown dwarfsen
dc.subjectStars: low-massen
dc.subjectStars: atmospheresen
dc.subjectInfrared: starsen
dc.subjectRadio lines: starsen
dc.subjectX-rays: starsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleAtmospheres of brown dwarfsen
dc.typeJournal itemen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1007/s00159-014-0080-0
dc.description.statusPeer revieweden
dc.date.embargoedUntil2015-11-16


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