CLES evolutionary tracks (alpha-enhanced)

Grid of evolutionary tracks with CLES (Scuflaire et al. 08). Version 19.2 (August 2019). Initial chemical composition:<br> - [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.<br> - [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. There is a directory for each initial chemical composition. Each of them contains the evolutionary track<br> (from ZAMS to RGB at 25Rsun) for stars with masses between 0.7 and 2.5 Msun (step: 0.02Msun). columns:<br> 1: age (yrs)<br> 2: log_Te<br> 3: log_L_Lsun<br> 4: Xc central Hydrogen mass fraction<br> 5: Yc central Helium mass fraction<br> 6: X0 Initial Hydrogen mass fraction<br> 7: Z0 Initial metal mass fraction<br> 8: Z/Hs metal over H in surface<br> 9: P0 2*pi**2/Int{N_BV/r*dr} (N_BV Brunt-Vaisala frequency)<br> 10: F0 asymptotic large frequency separation =1/2/Int{dr/c} (c: sound speed) Input physics:<br> Reference solar metal mixture: AGSS09<br> Solar stellar parameters (IAU2015)<br> Radiative opacity: OPAL at high temperature and Wichita University opacities at low temperature for the especific chemical composition. <br> EoS: Irwin (2003)<br> Nuclear reaction rates: Adelberg+2011 or Nacre if not available in Adelberg's compilation<br> Convection:MLT (Cox &amp; Giuli 68), mixing length parameter from solar calibration with same physics.<br> Extra-mixing: instantaneous overshooting over convective core (extra-mixing size=0.1Hp) and undershooting below convective envelope (extra-mixing size=0.2Hp)<br> Microscopic diffusion of H and He (Thoul et al. 94)