Volume 633, January 2020
|Number of page(s)||15|
|Section||Stellar structure and evolution|
|Published online||06 January 2020|
Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
2 IRAP, UMR 5277 CNRS and Université de Toulouse, 14, Av. E. Belin, 31400 Toulouse, France
3 Institut UTINAM, CNRS UMR 6213, Univ. Bourgogne Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, 25010 Besançon Cedex, France
4 UMR 5299 LUPM CNRS Université Montpellier II, Place Eugène Bataillon, 34095 Montpellier Cedex 05, France
5 Institute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
6 University of Texas, McDonald Observatory TX 79734, USA
7 National Optical Astronomy Observatory, Tucson, USA
8 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-176 Warsaw, Poland
9 Twitter, 1355 Market Street, Suite 900, San Francisco, CA 94103, USA
Accepted: 22 October 2019
Context. Li is extensively known to be a good tracer of non-standard mixing processes occurring in stellar interiors.
Aims. We present the results of a new large Li survey in red giant stars and combine it with surveys from the literature to probe the impact of rotation-induced mixing and thermohaline double-diffusive instability along stellar evolution.
Methods. We determined the surface Li abundance for a sample of 829 giant stars with accurate Gaia parallaxes for a large sub-sample (810 stars) complemented with accurate HIPPARCOS parallaxes (19 stars). The spectra of our sample of northern and southern giant stars were obtained in three ground-based observatories (Observatoire de Haute-Provence, ESO-La Silla, and the Mc Donald Observatory). We determined the atmospheric parameters (Teff, log(g) and [Fe/H]), and the Li abundance. We used Gaia parallaxes and photometry to determine the luminosity of our objects and we estimated the mass and evolution status of each sample star with a maximum-likelihood technique using stellar evolution models computed with the STAREVOL code. We compared the observed Li behaviour with predictions from stellar models, including rotation and thermohaline mixing. The same approach was used for stars from selected Li surveys from the literature.
Results. Rotation-induced mixing accounts nicely for the Li behaviour in stars warmer than about 4200 K, independently of the mass domain. For stars with masses lower than 2 M⊙ thermohaline mixing leads to further Li depletion below the Teff of the RGB bump (about 4000 K), and on the early asymptotic giant branch, as observed. Depending on the definition we adopt, we find between 0.8 and 2.2% of Li-rich giants in our new sample.
Conclusions.Gaia puts a new spin on the understanding of mixing processes in stars, and our study confirms the importance of rotation-induced processes and of thermohaline mixing. However asteroseismology is required to definitively pinpoint the actual evolution status of Li-rich giants.
Key words: stars: abundances / stars: evolution / surveys / stars: late-type
Full Tables 1 and 2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/633/A34
Based on observations made with the Aurélie spectrograph mounted on the 1.52m telescope at Observatoire de Haute-Provence (CNRS), France, with the FEROS spectrograph mounted on the MPI 2.2m telescope at ESO-La Silla Observatory (programmes 072.D-0235A, B; PI: C. Charbonnel), and with the Sandiford Cassegrain Echelle Spectrometer mounted on the Struve telescope at McDonald Observatory, Texas, USA.
© ESO 2020
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