The evolution through H and He burning of Galactic cluster stars

Details The evolution through H and He burning of Galactic cluster stars The evolution through H and He burning of Galactic cluster stars

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apjs...78..517c&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 78, Feb. 1992, p. 517-536.

Statistics

Computation

139

Globular Clusters, Metallicity, Stellar Evolution, Stellar Models, Color-Magnitude Diagram, Helium, Hydrogen, Red Giant Stars, Stellar Luminosity, Stellar Mass

Scientific paper

A set of theoretical computations for solar metallicity stellar models is presented, extending previous computations of intermediate-mass stars to lower masses, crossing the RGB phase transition, down to 1-solar-mass stars. Theoretical isochrones and synthetic clusters were produced in the range of ages between 30 and 11,000 Myr, covering the range of age spanned by the large majority of Galactic clusters. The variations among the relative frequencies of subgiants, red giants, and clump stars are not found to be strictly connected to the RGB phase transition. Although the RGB phase transition may be safely settled between 2 and 2.5 solar masses, the mass limit discriminating between clusters dominated by clump stars and those dominated by subgiant stars is of the order of 1.8 solar masses. In the range of ages between 0.6 and 10 Gyr, the luminosity of the central He-burning models is found to be almost insensitive to the age, supporting the use of clump stars to derive the cluster distance moduli.

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