The Gaia-ESO survey: Mixing processes in low-mass stars traced by lithium abundance in cluster and field stars

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dc.contributor.authorMagrini, L.
dc.contributor.authorLagarde, N.
dc.contributor.authorCharbonnel, C.
dc.contributor.authorFranciosini, E.
dc.contributor.authorRandich, S.
dc.contributor.authorSmiljanic, R.
dc.contributor.authorCasali, G.
dc.contributor.authorViscasillas Vázquez, C.
dc.contributor.authorSpina, L.
dc.contributor.authorBiazzo, K.
dc.contributor.authorPasquini, L.
dc.contributor.authorBragaglia, A.
dc.contributor.authorVan Der Swaelmen, M.
dc.contributor.authorTautvaišienė, G.
dc.contributor.authorInno, L.
dc.contributor.authorSanna, N.
dc.contributor.authorPrisinzano, L.
dc.contributor.authorDegl’Innocenti, S.
dc.contributor.authorPrada Moroni, P.
dc.contributor.authorRoccatagliata, V.
dc.contributor.authorTognelli, E.
dc.contributor.authorMonaco, L.
dc.contributor.authorDe Laverny, P.
dc.contributor.authorDelgado-Mena, E.
dc.contributor.authorBaratella, M.
dc.contributor.authorD’Orazi, V.
dc.contributor.authorVallenari, A.
dc.contributor.authorGonneau, A.
dc.contributor.authorWorley, C.
dc.contributor.authorJiménez-Esteban, F.
dc.contributor.authorJofre, P.
dc.contributor.authorBensby, T.
dc.contributor.authorFrançois, P.
dc.contributor.authorGuiglion, G.
dc.contributor.authorBayo, Amelia
dc.contributor.authorJeffries, R. D.
dc.contributor.authorBinks, A. S.
dc.contributor.authorGilmore, G.
dc.contributor.authorDamiani F.
dc.contributor.authorKorn, A.
dc.contributor.authorPancino, E.
dc.contributor.authorSacco, G. G.
dc.contributor.authorHourihane, A.
dc.contributor.authorMorbidelli, L.
dc.contributor.authorZaggia, S.
dc.date.accessioned2022-11-30T02:46:31Z
dc.date.available2022-11-30T02:46:31Z
dc.date.issued2021
dc.description.abstractAims. We aim to constrain the mixing processes in low-mass stars by investigating the behaviour of the Li surface abundance after the main sequence. We take advantage of the data from the sixth internal data release of Gaia-ESO, IDR6, and from the Gaia Early Data Release 3, EDR3s. Methods. We selected a sample of main-sequence, sub-giant, and giant stars in which the Li abundance is measured by the Gaia-ESO survey. These stars belong to 57 open clusters with ages from 130 Myr to about 7 Gyr and to Milky Way fields, covering a range in [Fe/H] between ∼​ − 1.0 and ∼​ + 0.5 dex, with few stars between ∼​ − 1.0 and ∼​ − 2.5 dex. We studied the behaviour of the Li abundances as a function of stellar parameters. We inferred the masses of giant stars in clusters from the main-sequence turn-off masses, and for field stars through comparison with stellar evolution models using a maximum likelihood technique. We compared the observed Li behaviour in field giant stars and in giant stars belonging to individual clusters with the predictions of a set of classical models and of models with mixing induced by rotation and thermohaline instability. Results. The comparison with stellar evolution models confirms that classical models cannot reproduce the observed lithium abundances in the metallicity and mass regimes covered by the data. The models that include the effects of both rotation-induced mixing and thermohaline instability account for the Li abundance trends observed in our sample in all metallicity and mass ranges. The differences between the results of the classical models and of the rotation models largely differ (up to 2 dex), making lithium the best element with which to constrain stellar mixing processes in low-mass stars. We discuss the nature of a sample of Li-rich stars. Conclusions. We demonstrate that the evolution of the surface abundance of Li in giant stars is a powerful tool for constraining theoretical stellar evolution models, allowing us to distinguish the effect of different mixing processes. For stars with well-determined masses, we find a better agreement of observed surface abundances and models with rotation-induced and thermohaline mixing. Rotation effects dominate during the main sequence and the first phases of the post-main-sequence evolution, and the thermohaline induced mixing after the bump in the luminosity function.en_ES
dc.facultadFacultad de Cienciasen_ES
dc.file.nameMagrini_Gai2021.pdf
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202140935
dc.identifier.urihttp://repositoriobibliotecas.uv.cl/handle/uvscl/7403
dc.languageen
dc.publisherEuropean Southern Observatory (ESO)
dc.rights© ESO 2021
dc.sourceAstronomy & Astrophysics
dc.subjectSTARS: ABUNDANCESen_ES
dc.subjectSTARS: EVOLUTIONen_ES
dc.subjectOPEN CLUSTERS AND ASSOCIATIONS: GENERALen_ES
dc.titleThe Gaia-ESO survey: Mixing processes in low-mass stars traced by lithium abundance in cluster and field stars
dc.typeArticulo
uv.departamentoInstituto de Fisica y Astronomia

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