========================================================================== J/MNRAS/298/525 Stellar evolution models for Z = 0.0001 to 0.03 (Pols+ 1998) The following files can be converted to FITS (extension .fit or fit.gz) ubvri_*.dat evgrid/ZAMS* summary.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/MNRAS/298/525 ==========================================================================
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Beginning of ReadMe : J/MNRAS/298/525 Stellar evolution models for Z = 0.0001 to 0.03 (Pols+ 1998) ================================================================================ Stellar evolution models for Z = 0.0001 to 0.03. Pols O.R., Schroeder K.-P., Hurley J.R., Tout C.A., Eggleton P.P. <Mon. Not. R. Astron. Soc., 298, 525-536 (1998)> =1998MNRAS.298..525P ================================================================================ ADC_Keywords: Models, evolutionary Keywords: convection - stars: evolution - Hertzsprung-Russell (HR) diagram - stars: population II - open clusters and associations: general - galaxies: stellar content Abstract: We have calculated a grid of empirically well tested evolutionary tracks with masses M between 0.5 and 50M_sun_, spaced by approximately 0.1 in log M, and with metallicities Z=0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02 and 0.03. We use a robust and fast evolution code with a self-adaptive non-Lagrangian mesh, which employs the mixing-length theory but treats convective mixing as a diffusion process, solving simultaneously for the structure and the chemical composition. The hydrogen and helium abundances are chosen as functions of the metallicity: X=0.76-3.0Z and Y=0.24+2.0Z. Two sets of models were computed, one without and one with a certain amount of enhanced mixing or 'overshooting'. Description: The results of the models studied in the paper are stored in the "evgrid" subdirectory, which includes for the metallicities/masses studied the ZAMS parameters and the evolutionary tracks computed with or without overshooting. A set of Fortran programs is also included which computes luminosities, radiuses, absolute magnitudes, and colors in the UBVRI Johnson-Cousins as a function of stellar age for any interpolation in the grid of models; a README file in this "evgrid" subdirectory gives details for an extended usage of the models.