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dc.contributor.authorBaraffe, I.
dc.contributor.authorHomeier, D.
dc.contributor.authorAllard, F.
dc.contributor.authorChabrier, G.
dc.date.accessioned2015-10-29T09:44:21Z
dc.date.issued2015-03-13
dc.description.abstractWe present new models for low-mass stars down to the hydrogen-burning limit that consistently couple atmosphere and interior structures, thereby superseding the widely used BCAH98 models. The new models include updated molecular linelists and solar abundances, as well as atmospheric convection parameters calibrated on 2D/3D radiative hydrodynamics simulations. Comparison of these models with observations in various colour-magnitude diagrams for various ages shows significant improvement over previous generations of models. The new models can solve flaws that are present in the previous ones, such as the prediction of optical colours that are too blue compared to M dwarf observations. They can also reproduce the four components of the young quadruple system LkCa 3 in a colour-magnitude diagram with one single isochrone, in contrast to any presently existing model. In this paper we also highlight the need for consistency when comparing models and observations, with the necessity of using evolutionary models and colours based on the same atmospheric structures.en_GB
dc.description.sponsorshipRoyal Societyen_GB
dc.description.sponsorshipERCen_GB
dc.description.sponsorshipconsolidated STFC granten_GB
dc.description.sponsorshipFrench ANR (GuEPARD)en_GB
dc.description.sponsorshipPNPS of the CNRS (INSU)en_GB
dc.identifier.citationVol. 577 (May 2015) A42en_GB
dc.identifier.doi10.1051/0004-6361/201425481
dc.identifier.grantnumberFP7/2007-2013 Grant Agreement No. 247060en_GB
dc.identifier.grantnumberST/J001627/1en_GB
dc.identifier.grantnumberANR10-BLANC0504-01en_GB
dc.identifier.grantnumberWM090065en_GB
dc.identifier.urihttp://hdl.handle.net/10871/18543
dc.language.isoenen_GB
dc.publisherEDP Sciencesen_GB
dc.relation.urlhttp://dx.doi.org/10.1051/0004-6361/201425481en_GB
dc.relation.urlhttp://arxiv.org/abs/1503.04107v1en_GB
dc.rightsCopyright © ESO, 2015en_GB
dc.subjectastro-ph.SRen_GB
dc.subjectastro-ph.SRen_GB
dc.subjectstars: evolutionen_GB
dc.subjectstars: low-massen_GB
dc.subjectstars: pre-main sequenceen_GB
dc.subjectHertzsprung-Russell and C-M diagramsen_GB
dc.subjectconvectionen_GB
dc.titleNew evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limiten_GB
dc.typeArticleen_GB
dc.date.available2015-10-29T09:44:21Z
dc.identifier.issn0004-6361
dc.identifier.journalAstronomy and Astrophysicsen_GB


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