The Gaia-ESO Survey: Stellar radii in the young open clusters NGC 2264, NGC 2547, and NGC 2516

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dc.contributor.authorJackson, R. J.
dc.contributor.authorJeffries, R. D.
dc.contributor.authorRandich, S.
dc.contributor.authorBragaglia, A.
dc.contributor.authorCarraro, G.
dc.contributor.authorCostado, M. T.
dc.contributor.authorFlaccomio, E.
dc.contributor.authorLanzafame, A. C.
dc.contributor.authorLardo, C.
dc.contributor.authorMonaco, L.
dc.contributor.authorMorbidelli, L.
dc.contributor.authorSmiljanic, R.
dc.contributor.authorZaggia, S.
dc.date.accessioned2017-08-17T14:40:57Z
dc.date.available2017-08-17T14:40:57Z
dc.date.issued2016-02
dc.descriptionIndexación: Web of Science; Scopus.es_CL
dc.description.abstractContext. Rapidly rotating, low-mass members of eclipsing binary systems have measured radii that are significantly larger than predicted by standard evolutionary models. It has been proposed that magnetic activity is responsible for this radius inflation. Aims. By estimating the radii of low-mass stars in three young clusters (NGC2264, NGC2547, NGC2516, with ages of similar to 5, similar to 35 and similar to 140Myr respectively), we aim to establish whether similar radius inflation is seen in single, magnetically active stars. Methods. We use radial velocities from the Gaia-ESO Survey (GES) and published photometry to establish cluster membership and then combine GES measurements of projected equatorial velocities with published rotation periods to estimate the average radii for groups of fast-rotating cluster members as a function of their luminosity and age. The average radii are compared with the predictions of both standard evolutionary models and variants that include magnetic inhibition of convection and starspots. Results. At a given luminosity, the stellar radii in NGC 2516 and NGC 2547 are larger than predicted by standard evolutionary models at the ages of these clusters. The discrepancy is least pronounced and not significant (similar to 10 per cent) in zero age main sequence stars with radiative cores, but more significant in lower-mass, fully convective pre main-sequence cluster members, reaching similar to 30 similar to 10 per cent. The uncertain age and distance of NGC 2264 preclude a reliable determination of any discrepancy for its members. Conclusions. The median radii we have estimated for low-mass fully convective stars in the older clusters are inconsistent (at the 2-3 sigma level) with non-magnetic evolutionary models and more consistent with models that incorporate the effects of magnetic fields or dark starspots. The available models suggest this requires either surface magnetic fields exceeding 2.5 kG, spots that block about 30 per cent of the photospheric flux, or a more moderate combination of both.es_CL
dc.description.urihttps://www.aanda.org/articles/aa/abs/2016/02/aa27507-15/aa27507-15.html
dc.identifier.citationAstronomy and Astrophysics Volume 586, 1 February 2016, Article number A52es_CL
dc.identifier.issn1432-0746
dc.identifier.otherhttps://doi.org/10.1051/0004-6361/201527507
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/3958
dc.language.isoenes_CL
dc.publisherEDP SCIENCESes_CL
dc.subjectStars: rotationes_CL
dc.subjectStars: low-masses_CL
dc.subjectStars: activityes_CL
dc.subjectOpen clusters and associations: individual: NGC 2264es_CL
dc.subjectOpen clusters and associations: individual: NGC 2547es_CL
dc.subjectOpen clusters and associations: individual: NGC 2516es_CL
dc.titleThe Gaia-ESO Survey: Stellar radii in the young open clusters NGC 2264, NGC 2547, and NGC 2516es_CL
dc.typeArtículoes_CL
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