Dataset Open Access

CLES evolutionary tracks (alpha-enhanced)

Montalban, Josefina; Noel, Arlette; Scuflaire, Richard


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    <subfield code="a">&lt;p&gt;Grid of evolutionary tracks with CLES (Scuflaire et al. 08). Version 19.2 (August 2019).&lt;/p&gt;

&lt;p&gt;Initial chemical composition:&lt;br&gt;
- [alpha/Fe]=0.0, +0.1, +0.2, +0.3, +0.4 and, for each alpha enhancement: 23 different values of [Fe/H], from -2.5 to +0.25, with steps of 0.1 or 0.15 dex.&lt;br&gt;
- [alpha/Fe]=-0.1, +0.5, +0.6, eight different values of [Fe/H]: from -1.50 to +0.25 with step 0.25 dex.&lt;/p&gt;

&lt;p&gt;There is a directory for each initial chemical composition. Each of them contains the evolutionary track&lt;br&gt;
(from ZAMS to RGB at 25Rsun) for stars with masses between 0.7 and 2.5 Msun (step: 0.02Msun).&lt;/p&gt;

&lt;p&gt;columns:&lt;br&gt;
1:&amp;nbsp; age (yrs)&lt;br&gt;
2:&amp;nbsp; log_Te&lt;br&gt;
3:&amp;nbsp; log_L_Lsun&lt;br&gt;
4:&amp;nbsp; Xc central Hydrogen mass fraction&lt;br&gt;
5:&amp;nbsp; Yc central Helium&amp;nbsp; mass fraction&lt;br&gt;
6:&amp;nbsp; X0 Initial Hydrogen mass fraction&lt;br&gt;
7:&amp;nbsp; Z0 Initial metal mass fraction&lt;br&gt;
8:&amp;nbsp; Z/Hs metal over H in surface&lt;br&gt;
9:&amp;nbsp; P0 2*pi**2/Int{N_BV/r*dr} (N_BV Brunt-Vaisala frequency)&lt;br&gt;
10: F0 asymptotic large frequency separation =1/2/Int{dr/c} (c: sound speed)&lt;/p&gt;

&lt;p&gt;Input physics:&lt;br&gt;
Reference solar metal mixture: AGSS09&lt;br&gt;
Solar stellar parameters (IAU2015)&lt;br&gt;
Radiative opacity: OPAL at high temperature and&amp;nbsp; Wichita University opacities at low temperature for the especific chemical composition.&amp;nbsp;&amp;nbsp;&amp;nbsp;&amp;nbsp;&amp;nbsp;&amp;nbsp; &amp;nbsp;&lt;br&gt;
EoS: Irwin (2003)&lt;br&gt;
Nuclear reaction rates: Adelberg+2011 or Nacre if not available in Adelberg&amp;#39;s compilation&lt;br&gt;
Convection:MLT (Cox &amp;amp; Giuli 68), mixing length parameter from solar calibration with same physics.&lt;br&gt;
Extra-mixing: instantaneous overshooting over convective core (extra-mixing size=0.1Hp) and undershooting below convective envelope (extra-mixing size=0.2Hp)&lt;br&gt;
Microscopic diffusion of H and He (Thoul et al. 94)&lt;/p&gt;

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