English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present an extended grid of state-of-the art stellar models for low-massstars including updated physics (nuclear reaction rates, surface boundarycondition, mass-loss rate, angular momentum transport, torque androtation-induced mixing prescriptions).  We aim at evaluating the impact of wind braking, realistic atmospherictreatment, rotation and rotation-induced mixing on the structural androtational evolution from the pre-main sequence to the turn-off.  Using the STAREVOL code, we provide an updated PMS grid. We compute stellarmodels for 7 different metallicities, from [Fe/H] = -1 dex to [Fe/H] = +0.3 dexwith a solar composition corresponding to $Z=0.0134$. The initial stellar massranges from 0.2 to 1.5\Ms with extra grid refinement around one solar mass. Wealso provide rotating models for three different initial rotation rates (slow,median and fast) with prescriptions for the wind braking and disc-couplingtimescale calibrated on observed properties of young open clusters. Therotational mixing includes an up-to-date description of the turbulenceanisotropy in stably stratified regions.  The overall behaviour of our models at solar metallicity -- and itsconstitutive physics -- is validated through a detailed comparison with avariety of distributed evolutionary tracks. The main differences arise from thechoice of surface boundary conditions and initial solar composition.  The models including rotation with our prescription for angular momentumextraction and self-consistent formalism for angular momentum transport areable to reproduce the rotation period distribution observed in young openclusters over a broad mass-range.  These models are publicly available and may be used to analyse data comingfrom present and forthcoming asteroseismic and spectroscopic surveys such asGaia, TESS and PLATO.

astronomy and astrophysics

First grids of low-mass stellar models and isochrones with  self-consistent treatment of rotation : From 0.2 to 1.5 M_\odot at 7  metallicities from PMS to TAMS