J/A+A/631/A77ivo://CDS.VizieR/J/A+A/631/A77doi:10.26093/cds/vizier.36310077CDSAmard L.Palacios A.Charbonnel C.Gallet F.Georgy C.Lagarde N.,Siess L.2019-10-22T09:32:10Z2019-10-22T10:31:13ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frstellar-evolutionary-modelsstellar-evolutionary-trackspre-main-sequence-starsWe 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. Using the STAREVOL code, we provide an updated PMS grid. We computed stellar models for seven different metallicities, from [Fe/H]=-1dex to [Fe/H]=+0.3dex with a solar composition corresponding to Z=0.0134. The initial stellar mass ranges from 0.2 to 1.5M_{sun}_ 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. 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.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.2019A&A...631A..77Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/631/A77CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/631/A77https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/631/A77http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/631/A77https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/631/A77https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/631/A77http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/631/A77GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/631/A77/listList of all the tracks and isochrone filesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMini[0.20/1.50]? Initial mass (for tracks only) (1)solMassphys.massfloatnullableZini[0.0002/0.0260] Initial metallicity (2)phys.abund.ZfloatVini[0.00/0.60] Initial rotation rate (3)phys.energyfloatlogT[6.0/10.1]? Initial age (for isochrones only) (4)log(yr)time.agefloatnullableFileNameName of the filemeta.id;meta.filechar