Volume 631, November 2019
|Number of page(s)||21|
|Section||Stellar structure and evolution|
|Published online||22 October 2019|
First grids of low-mass stellar models and isochrones with self-consistent treatment of rotation
From 0.2 to 1.5 M⊙ at seven metallicities from PMS to TAMS⋆
Department of Astronomy – University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
2 LUPM UMR 5299 CNRS/UM, Université de Montpellier, CC 72, 34095 Montpellier Cedex 05, France
3 University of Exeter, Department of Physics & Astronomy, Stoker Road, Devon, Exeter EX4 4QL, UK
4 IRAP, UMR 5277 CNRS and Université de Toulouse, 14 Av. E. Belin, 31400 Toulouse, France
5 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
6 Institut UTINAM, CNRS UMR 6213, Univ. Bourgogne Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, 25010 Besançon Cedex, France
7 Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB), CP226, Boulevard du Triomphe, 1050 Brussels, Belgium
Accepted: 20 May 2019
Aims. We present an extended grid of state-of-the art stellar models for low-mass stars including updated physics (nuclear reaction rates, surface boundary condition, mass-loss rate, angular momentum transport, rotation-induced mixing, and torque prescriptions). We evaluate the impact of wind braking, realistic atmospheric treatment, rotation, and rotation-induced mixing on the structural and rotational evolution from the pre-main sequence (PMS) to the turn-off.
Methods. Using the STAREVOL code, we provide an updated PMS grid. We computed stellar models for seven different metallicities, from [Fe/H] = −1 dex to [Fe/H] = +0.3 dex with a solar composition corresponding to Z = 0.0134. The initial stellar mass ranges from 0.2 to 1.5 M⊙ with extra grid refinement around one solar mass. We also provide rotating models for three different initial rotation rates (slow, median, and fast) with prescriptions for the wind braking and disc-coupling timescale calibrated on observed properties of young open clusters. The rotational mixing includes the most recent description of the turbulence anisotropy in stably stratified regions.
Results. The overall behaviour of our models at solar metallicity, and their constitutive physics, are validated through a detailed comparison with a variety of distributed evolutionary tracks. The main differences arise from the choice of surface boundary conditions and initial solar composition. The models including rotation with our prescription for angular momentum extraction and self-consistent formalism for angular momentum transport are able to reproduce the rotation period distribution observed in young open clusters over a wide range of mass values. These models are publicly available and can be used to analyse data coming from present and forthcoming asteroseismic and spectroscopic surveys such as Gaia, TESS, and PLATO.
Key words: stars: evolution / stars: rotation / stars: low-mass / stars: pre-main sequence
The model grid is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A77
© ESO 2019
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