Evolution of low mass stars through mass loss - Transition from the main sequence to the degenerate phase

Details Evolution of low mass stars through mass loss - Transition from the main sequence to the degenerate phase Evolution of low mass stars through mass loss - Transition from the main sequence to the degenerate phase

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...113..303d&link_type=abstract

Astronomy and Astrophysics, vol. 113, no. 2, Sept. 1982, p. 303-310.

Astronomy and Astrophysics

Astrophysics

21

Binary Stars, Dwarf Stars, Main Sequence Stars, Stellar Evolution, Stellar Mass Ejection, Abundance, Hertzsprung-Russell Diagram, Mass To Light Ratios, Nuclear Reactions, Stellar Luminosity, Stellar Structure

Scientific paper

The constant rate mass loss evolution of low mass stars is traced from the case of fully convective structures of about 0.2 solar masses to mass values at which nuclear energy sources are no longer able to support the stellar structure. It is noted that the sudden onset of pressure ionization in stars of less than about 0.1 solar masses, and the consequent uncertainty in the adiabatic gradient in the region in which covolume effects are dominant, cause a nonnegligible uncertainty in the determination of the central temperature of the star. The mass-luminosity relation is presented as a function of the He and metal content, and the relation's application to the construction of the luminosity function of red and black dwarfs is outlined. It is suggested that some stars close to the main sequence lower mass limit may lose an important fraction of their mass during the galactic lifetime, and die as black dwarfs.

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