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dc.contributor.authorBaraffe, I
dc.contributor.authorElbakyan, VG
dc.contributor.authorVorobyov, EI
dc.contributor.authorChabrier, G
dc.date.accessioned2016-11-09T09:53:39Z
dc.date.issued2016-08-26
dc.description.abstractWe present self-consistent calculations coupling numerical hydrodynamics simulations of collapsing pre-stellar cores and stellar evolution models of accreting objects. We analyse the main impact of consistent accretion history on the evolution and lithium depletion of young low-mass stars and brown dwarfs. These consistent models confirm the generation of a luminosity spread in Herzsprung-Russell diagrams at ages $\sim$ 1-10 Myr. They also confirm that early accretion can produce objects with abnormal Li depletion, as found in a previous study that was based on arbitrary accretion rates. The results strengthen that objects with anomalously high level of Li depletion in young clusters should be extremely rare. We also find that early phases of burst accretion can produce coeval models of similar mass with a range of different Li surface abundances, and in particular with Li-excess compared to the predictions of non-accreting counterparts. This result is due to a subtle competition between the effect of burst accretion and its impact on the central stellar temperature, the growth of the stellar radiative core and the accretion of fresh Li from the accretion disk. Only consistent models could reveal such a subtle combination of effects. This new result could explain the recent, puzzling observations of Li-excess of fast rotators in the young cluster NGC 2264. Present self-consistent accreting models are available in electronic form.en_GB
dc.description.sponsorshipWe thanks Amelia Bayo, Min Fang and Laura Venuti for providing their data. This project was partly supported by the European Research Council through grants ERC- AdG No. 320478-TOFU and No. 247060-PEPS, by the Russian Ministry of Education and Science Grant 3.961.2014/K and by the Austrian Science Fund (FWF) under research grant I2549- N27. V.G.E. acknowledges Southern Federal University Development Program for nancial support. The simulations were performed on the Vienna Scienti c Cluster (VSC-2), on the Shared Hierarchical Academic Research Computing Network (SHARCNET), on the Atlantic Computational Excellence Network (ACEnet) and on the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS and the University of Exeter.en_GB
dc.identifier.citationarXiv:1608.07428 [astro-ph.SR]en_GB
dc.identifier.urihttp://hdl.handle.net/10871/24348
dc.language.isoenen_GB
dc.publisherarXiv.orgen_GB
dc.relation.urlhttp://arxiv.org/abs/1608.07428v1en_GB
dc.rightsThis is the author accepted manuscript.
dc.subjectastro-ph.SRen_GB
dc.subjectastro-ph.SRen_GB
dc.titleSelf-consistent evolution of accreting low-mass stars and brown dwarfsen_GB
dc.typeArticleen_GB
dc.date.available2016-11-09T09:53:39Z
dc.description14 pages, 8 figures, accepted for publication in Astronomy and Astrophysicsen_GB
dc.identifier.journalarXiven_GB


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