/ftp/cats/J/MNRAS/298/525



==========================================================================
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
==========================================================================

drwxr-xr-x 7 cds cds 4096 Jan 29 2012 [Up] drwxr-xr-x 3 cds cds 4096 Jul 12 12:35 [TAR file] -rw-r--r-- 1 cds cds 492 Jul 12 12:35 .message -r--r--r-- 1 cds cds 7984 Jul 12 2009 ReadMe drwxr-xr-x 2 cds cds 4096 Apr 25 2009 evgrid -r--r--r-- 1 cds cds 491912 Apr 25 2009 summary.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cds cds 320136 Apr 25 2009 ubvri_c.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cds cds 320136 Apr 25 2009 ubvri_k.dat [txt] [txt.gz] [fits] [fits.gz] [html]
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.

© UDS/CNRS

Contact