A&A Supplement series, Vol. 128, March II 1998, 471-474
Received February 6; accepted July 22, 1997
N. Mowlavi, D. Schaerer, G. Meynet, P.A. Bernasconi, C. Charbonnel, and A. Maeder
Send offprint request: N. Mowlavi
Geneva Observatory, CH-1290 Sauverny, Switzerland
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A.
Laboratoire d'Astrophysique de Toulouse, CNRS - UMR 5572, 14 Av. E. Belin, 31400 Toulouse, France
We present a new grid of stellar models from 0.8 to at Z=0.10, with mass loss and moderate overshooting, from the zero age main sequence to either the helium flash (low mass stars), the early AGB phase (intermediate-mass stars) or the end of carbon burning (massive stars). The calculations are done with opacities provided by Iglesias & Rogers (1993), completed by those of Alexander & Ferguson (1994) at low temperatures. This grid is a homogeneous extension to very high metallicity of the previous grids published by the Geneva group. It is useful for the study of galactic bulges, elliptical galaxies and eventually quasars. Calculations of stars more massive than are not presented as these objects lose almost their entire mass during their main sequence phase, and are likely to end their life as white dwarfs.
keywords: stars: evolution -- stars: Hertzsprung-Russell diagram -- stars: interiors