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Issue
Astron. Astrophys. Suppl. Ser.
Volume 128, Number 3, March II 1998
Page(s) 471 - 474
DOI http://dx.doi.org/10.1051/aas:1998388
DOI: 10.1051/aas:1998388

A&A Supplement series, Vol. 128, March II 1998, 471-474

Received February 6; accepted July 22, 1997

Grids of stellar models

VII. From 0.8 to 60 tex2html_wrap_inline569 at tex2html_wrap_inline571 = 0.10gif

N. Mowlavitex2html_wrap593, D. Schaerertex2html_wrap595, G. Meynettex2html_wrap593, P.A. Bernasconitex2html_wrap593, C. Charbonneltex2html_wrap601, and A. Maedertex2html_wrap593

Send offprint request: N. Mowlavi

tex2html_wrap605  Geneva Observatory, CH-1290 Sauverny, Switzerland
tex2html_wrap607  Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A.
tex2html_wrap609  Laboratoire d'Astrophysique de Toulouse, CNRS - UMR 5572, 14 Av. E. Belin, 31400 Toulouse, France

Abstract:

We present a new grid of stellar models from 0.8 to tex2html_wrap_inline575 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 tex2html_wrap_inline575 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

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