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Resource Record Summary

Catalog Service:
Low-mass stellar models and isochrones

Short name: J/A+A/631/A77
IVOA Identifier: ivo://CDS.VizieR/J/A+A/631/A77
DOI (Digital Object Identifier): 10.26093/cds/vizier.36310077
Publisher: CDSivo://CDS[Pub. ID]
More Info: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/631/A77
VO Compliance: Level 2: This is a VO-compliant resource.
Status: active
Registered: 2019 Oct 22 10:31:13Z
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Description


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. 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.

More About this Resource

About the Resource Providers

This section describes who is responsible for this resource

Publisher: CDSivo://CDS[Pub. ID]

Creators:
Amard L.Palacios A.Charbonnel C.Gallet F.Georgy C.Lagarde N.Siess L.

Contact Information:
X CDS support team
Email: cds-question at unistra.fr
Address: CDS
Observatoire de Strasbourg
11 rue de l'Universite
F-67000 Strasbourg
France

Status of This Resource

This section provides some status information: the resource version, availability, and relevant dates.

Version: n/a
Availability: This is an active resource.
  • This service provides only public data.
Relevant dates for this Resource:
  • Updated: 2019 Oct 22 09:32:10Z
  • Created: 2019 Oct 22 10:31:13Z

This resource was registered on: 2019 Oct 22 10:31:13Z
This resource description was last updated on: 2021 Oct 21 00:00:00Z

What This Resource is About

This section describes what the resource is, what it contains, and how it might be relevant.

Resource Class: CatalogService
This resource is a service that provides access to catalog data. You can extract data from the catalog by issuing a query, and the matching data is returned as a table.
Resource type keywords:
  • Catalog
Subject keywords:
  • Stellar evolutionary tracks
  • Stellar evolutionary models
  • Astronomical models
  • Pre-main sequence stars
Intended audience or use:
  • Research: This resource provides information appropriate for supporting scientific research.
More Info: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/631/A77 Literature Reference: 2019A&A...631A..77A

Related Resources:

Other Related Resources
TAP VizieR generic service(IsServedBy) ivo://CDS.VizieR/TAP [Res. ID]

Data Coverage Information

This section describes the data's coverage over the sky, frequency, and time.

Rights and Usage Information

This section describes the rights and usage information for this data.

Rights:

Available Service Interfaces

Custom Service

This is service that does not comply with any IVOA standard but instead provides access to special capabilities specific to this resource.

VO Compliance: Level 2: This is a VO-compliant resource.
Available endpoints for this service interface:
Custom Service

This is service that does not comply with any IVOA standard but instead provides access to special capabilities specific to this resource.

VO Compliance: Level 2: This is a VO-compliant resource.
Available endpoints for this service interface:
  • URL-based interface: http://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/631/A77
Table Access Protocol - Auxiliary ServiceXX

This is a standard IVOA service that takes as input an ADQL or PQL query and returns tabular data.

VO Compliance: Level 2: This is a VO-compliant resource.
Available endpoints for the standard interface:
  • http://tapvizier.cds.unistra.fr/TAPVizieR/tap


Developed with the support of the National Science Foundation
under Cooperative Agreement AST0122449 with the Johns Hopkins University
The NAVO project is a member of the International Virtual Observatory Alliance

This NAVO Application is hosted by the Space Telescope Science Institute

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