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dc.contributor.authorBaraffe, I
dc.contributor.authorChabrier, G
dc.date.accessioned2018-11-19T13:41:04Z
dc.date.issued2018-11-22
dc.description.abstractRecently, Jao et al. (2018) discovered a gap in the mid-M dwarfs main sequence revealed by the analysis of Gaia data Release 2. They suggested the feature is linked to the onset of full convection in M dwarfs. Following the announcement of this discovery, MacDonald & Gizis (2018) proposed an explanation based on standard stellar evolution models. In this paper we re-examine the explanation suggested by MacDonald & Gizis (2018). We confirm that nuclear burning and mixing process of $^3$He provide the best explanation for the observed feature. We also find that a change in the energy transport from convection to radiation does not induce structural changes that could be visible. Regarding the very details of the process, however, we disagree with MacDonald & Gizis (2018) and propose a different explanation.en_GB
dc.description.sponsorshipWe thank Christian Knigge, Russel White and Wei-Chun Jao for very useful discussions. This work is partly supported by the consolidated STFC grant ST/R000395/1 and the ERC grant No. 787361-COBOM.en_GB
dc.identifier.citationVol. 619 (A177). Published online 22 November 2018.en_GB
dc.identifier.doi10.1051/0004-6361/201834062
dc.identifier.urihttp://hdl.handle.net/10871/34819
dc.language.isoenen_GB
dc.publisherEDP Sciencesen_GB
dc.rights© ESO 2018.
dc.subjectlow-massen_GB
dc.subjectstars: evolutionen_GB
dc.subjectstars: pre-main sequenceen_GB
dc.subjectstars: Hertzsprung-Russell diagrams and Color-Magnitude diagramsen_GB
dc.subjectconvectionen_GB
dc.titleA closer look at the transition between fully convective and partly radiative low mass starsen_GB
dc.typeArticleen_GB
dc.identifier.issn0004-6361
dc.descriptionThis is the author accepted manuscript. The final version is available from EDP Sciences via the DOI in this record.en_GB
dc.identifier.journalAstronomy and Astrophysicsen_GB
refterms.dateFOA2018-12-20T09:21:59Z


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