Evolutionary models for low and intermediate mass stars with convective overshooting

Details Evolutionary models for low and intermediate mass stars with convective overshooting Evolutionary models for low and intermediate mass stars with convective overshooting

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26as...66..191b&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 66, no. 2, Nov. 1986, p. 191-234. CNR-supported research.

Physics

172

Astronomical Catalogs, Convection, Stellar Cores, Stellar Evolution, Stellar Models, Stellar Physics, A Stars, Asymptotic Giant Branch Stars, B Stars, Globular Clusters, Hertzsprung-Russell Diagram, Red Giant Stars

Scientific paper

Detailed numerical tabulations are provided for two sets of sequences of intermediate-mass stars whose evolution has been followed till advanced stages. These are the red-giant tip, the start of the thermally pulsing AGB phase, and core C-ignition according to the initial mass of the stars. The models span the range of initial mass 1.2 to 9 solar mass and have metal contents Z = 0.001 and Z = 0.020, assuming X = 0.700. The major novelty with respect to other computations (Becker, 1981; VandenBerg, 1985) is the inclusion of convective overshooting during core H and He burning phases, according to the prescription given by Bressan et al. (1981). Among others, one of the most important results of these computations is that the critical initial masses, below which core He-flash and C-ignition in highly degenerate material occur are now significantly lower than in classic models. The information contained in the tables can be applied to a large variety of astrophysical problems. In particular, it can be used in the study of the HR diagrams of young and intermediate-age star clusters.

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