Luminosity functions for very low mass stars and brown dwarfs

Details Luminosity functions for very low mass stars and brown dwarfs Luminosity functions for very low mass stars and brown dwarfs

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403..303l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 403, no. 1, p. 303-314.

Astronomy and Astrophysics

Astrophysics

26

Brown Dwarf Stars, Stellar Luminosity, Stellar Mass, Hertzsprung-Russell Diagram, M Stars, Solar Neighborhood, Star Clusters, Stellar Evolution, Stellar Models, White Dwarf Stars

Scientific paper

A theoretical investigation of the luminosity function for low-mass objects to constrain the stellar initial mass function at the low-mass end is reported. The ways in which luminosity functions for low-mass stars are affected by star formation histories, brown dwarf and premain-sequence cooling rates and main-sequence mass luminosity relations, and the IMF are examined. Cooling rates and the mass-luminosity relation are determined through a new series of evolutionary calculations for very low mass stars and brown dwarfs in the range 0.05-0.50 solar mass. Model luminosity functions are constructed for specific comparison with the results of four recent observational surveys. The likelihood that the stellar mass function in the solar neighborhood is increasing at masses near the bottom of the main sequence and perhaps at lower masses is confirmed. In the most optimistic case, brown dwarfs contribute half of the local missing disk mass. The actual contribution is likely to be considerably less.

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