The globular cluster metallicity scale - Evidence from stellar models

Details The globular cluster metallicity scale - Evidence from stellar models The globular cluster metallicity scale - Evidence from stellar models

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..154d&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 154-158.

Astronomy and Astrophysics

Astrophysics

28

Abundance, Atmospheric Models, Globular Clusters, Metallic Stars, Stellar Atmospheres, Stellar Models, Hertzsprung-Russell Diagram, Hydrodynamics, Stellar Temperature

Scientific paper

Theoretical giant branches have been constructed to determine their relative positions for metallicities in the Fe/H ratio range of -2.3 to zero. The models included the following improvements over previous studies: (1) in the convection zone, use of the variable mixing length formalism of Deupree and Varner (1980) in conjunction with Deupree's (1979) horizontally averaged opacity; (2) for the surface boundary conditions, a fit to the grid of model atmospheres of Bell et al. (1976). A relation between the Fe/H ratio and (B-V)o,g based on these models is presented which yields good agreement over the observed range of metallicities for galactic globular clusters and old disk clusters. The metallicity of 47 Tuc and M71 given by this calibration is about -0.8 dex.

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