Magrini, L, Lagarde, N, Charbonnel, C, Franciosini, E, Randich, S, Smiljanic, R, Casali, G, Vazquez, CV, Spina, L, Biazzo, K, Pasquini, L, Bragaglia, A, Swaelmen, MVD, Tautvaisiene, G, Inno, L, Sanna, N, Prisinzano, L, Degl'Innocenti, S, Moroni, PP, Roccatagliata, V, Tognelli, E, Monaco, L, Laverny, PD, Delgado-Mena, E, Baratella, M, D'Orazi, V, Vallenari, A, Gonneau, A, Worley, C, Jimenez-Esteban, F, Jofre, P, Bensby, T, Francois, P, Guiglion, G, Bayo, A, Jeffries, RD, Binks, AS, Korn, A, Gilmore, G, Damiani, F, Pancino, E, Sacco, GG, Hourihane, A, Morbidelli, L and Zaggia, S (2021) The Gaia-ESO survey: Mixing processes in low-mass stars traced by lithium abundance in cluster and field stars. Astronomy & Astrophysics, 651 (A84). ISSN 0004-6361

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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, edr3. We select a sample of main sequence, sub-giant, and giant stars in which Li abundance is measured by the Gaia-ESO survey, belonging to 57 open clusters with ages from 120~Myr to about 7 Gyr and to Milky Way fields, covering a range in [Fe/H] between -1.0 and +0.5dex. We study the behaviour of the Li abundances as a function of stellar parameters. We compare 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. The comparison with stellar evolution models confirms that classical models cannot reproduce the lithium abundances observed 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 to constrain stellar mixing processes in low-mass stars. For stars with well-determined masses, we find a better agreement between observed surface abundances and models with rotation-induced and thermohaline mixings, the former dominating during the main sequence and the first phases of the post-main sequence evolution and the latter after the bump in the luminosity function.

Item Type: Article
Additional Information: The final version of this article and all relevant information related to it, including copyrights, can be found online on the publishers website at;
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Humanities and Social Sciences > School of Social Science and Public Policy
Related URLs:
Depositing User: Symplectic
Date Deposited: 14 May 2021 10:24
Last Modified: 21 Sep 2021 14:18

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