The mass and luminosity of cool dwarf stars

Details The mass and luminosity of cool dwarf stars The mass and luminosity of cool dwarf stars

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.155..241b&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 155, no. 2, May 1989, p. 241-248.

Astronomy and Astrophysics

Astrophysics

4

Binary Stars, Cool Stars, Dwarf Stars, Mass To Light Ratios, Stellar Luminosity, Stellar Mass, Least Squares Method, Main Sequence Stars, Stellar Magnitude

Scientific paper

An empircal mass-luminosity relation is derived for main-sequence stars in the range where log m is between -0.6 and +0.1. The sample used in the computations is a combination of the visual double stars considered by Cester et al. (1983) and the spectroscopic binaries studied by Duquennoy and Mayor (1988). Linear and second-order fits were applied to these measures with rms errors of + or - 0.3 in magnitude and + or - 0.025 in the logarithm of stellar mass. An example is presented in which the relation is applied to the luminosity function of nearby stars.

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