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

TL;DR

This study uses Gaia-ESO and Gaia data to analyze lithium abundances in low-mass stars across various evolutionary stages and metallicities, revealing that models including rotation and thermohaline mixing best explain observed trends.

Contribution

It demonstrates that classical stellar models cannot reproduce lithium observations, while models with rotation and thermohaline mixing accurately match the data across different metallicities and masses.

Findings

Classical models fail to match observed lithium abundances.

Models with rotation and thermohaline mixing explain lithium trends.

Lithium is a key element to constrain stellar mixing processes.

Abstract

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.