Evolution of very low mass stars and brown dwarfs. II - The population II

Details Evolution of very low mass stars and brown dwarfs. II - The population II Evolution of very low mass stars and brown dwarfs. II - The population II

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..653d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 15, 1987, p. 653-662.

Astronomy and Astrophysics

Astrophysics

63

Brown Dwarf Stars, Globular Clusters, Opacity, Stellar Evolution, Stellar Luminosity, Stellar Mass, Main Sequence Stars, Mass To Light Ratios

Scientific paper

This paper addresses a number of problems connected with the evolution of low-mass (M ≤ 0.8 M_sun;) and very low mass (M ≥ 0.07 M_sun;) stars having metal contents much smaller than the solar metal content. Two main chemical compositions bracketing the Population II regime are considered: helium and metal contents Y = 0.23, Z = 10-4 (Cox and Stewart opacities) and Y = 0.25, Z = 10-3 (Alexander, Johnson, and Rypma opacities). For these compositions, the hydrogen burning minimum mass is evaluated. It is confirmed that the atmospheric opacities are the main factor influencing the minimum main-sequence luminosity. Population II luminosity functions (LFs) are constructed and applied to the interpretation of globular cluster main-sequence LFs.

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