Free access
Issue
Astron. Astrophys. Suppl. Ser.
Volume 135, Number 3, March II 1999
Page(s) 405 - 413
DOI http://dx.doi.org/10.1051/aas:1999454
DOI: 10.1051/aas:1999454

Astron. Astrophys. Suppl. Ser. 135, 405-413

Grids of stellar models

VIII. From 0.4 to 1.0 ${M_{\odot}}$ at Z=0.020 and Z=0.001, with the MHD equation of state[*]

C. Charbonnel 1,2 - W. Däppen 3 - D. Schaerer 1,2 - P.A. Bernasconi 4 - A. Maeder 4 - G. Meynet 4 - N. Mowlavi 4

Send offprint request: C. Charbonnel


1 - Laboratoire d'Astrophysique de Toulouse, CNRS UMR 5572, 14 Av. E. Belin, 31400 Toulouse, France
2 - Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A.
3 - Department of Physics and Astronomy, University of Southern California, Los Angeles, CA 90089-1342, U.S.A.
4 - Geneva Observatory, CH-1290 Sauverny, Switzerland

Received March 13, 1997; accepted October 23, 1998

Abstract:

We present stellar evolutionary models covering the mass range from 0.4 to 1 ${M_{\odot}}$ calculated for metallicities Z=0.020 and 0.001 with the MHD equation of state (Hummer & Mihalas 1988; Mihalas et al. 1988; Däppen et al. 1988). A parallel calculation using the OPAL (Rogers et al. 1996) equation of state has been made to demonstrate the adequacy of the MHD equation of state in the range of 1.0 to 0.8 ${M_{\odot}}$ (the lower end of the OPAL tables). Below, down to 0.4 ${M_{\odot}}$, we have justified the use of the MHD equation of state by theoretical arguments and the findings of Chabrier & Baraffe (1997).

We use the radiative opacities by Iglesias & Rogers (1996), completed with the atomic and molecular opacities by Alexander & Fergusson (1994). We follow the evolution from the Hayashi fully convective configuration up to the red giant tip for the most massive stars, and up to an age of 20 Gyr for the less massive ones. We compare our solar-metallicity models with recent models computed by other groups and with observations.

The present stellar models complete the set of grids computed with the same up-to-date input physics by the Geneva group (Z=0.020 and 0.001, Schaller et al. 1992; Bernasconi 1996, and Charbonnel et al. 1996; Z=0.008, Schaerer et al. 1992; Z=0.004, Charbonnel et al. 1993; Z=0.040, Schaerer et al. 1993; Z=0.10, Mowlavi et al. 1998; enhanced mass loss rate evolutionary tracks, Meynet et al. 1994).

Key words: stars: evolution -- stars: Hertzsprung-russell diagram -- stars: interiors -- stars: low-mass


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