The empirical mass-luminosity relation

Details The empirical mass-luminosity relation The empirical mass-luminosity relation

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..96..125c&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 96, no. 1, Oct. 1983, p. 125-140. Research supported by the Consiglio Nazi

Astronomy and Astrophysics

Astrophysics

22

Binary Stars, Main Sequence Stars, Mass To Light Ratios, Stellar Mass, Orbital Elements, Stellar Spectrophotometry

Scientific paper

The empirical mass-luminosity relation (MLR) main-sequence stars is reevaluated statistically on the basis of recent observations of spectroscopic and visual binary systems. The orbital elements and fractional-mass data for 107 visual systems collected from the literature, for the 45 visual systems selected for further study, and for 40 spectrophotometric detached main-sequence systems are presented in tables. The absolute visual magnitudes of the visual binaries are converted to bolometric magnitudes using the data of Johnson (1966). The data are plotted, and the MLR is found to be well defined only for the mass range 0.8-3 solar mass. The exponent alpha in the power-law MLR (L varies as M to the alpha) is calculated in three linear regressions as 3.05 + or - 0.14, 4.76 + or - 0.01, and 3.68 + or - 0.05 for stars of less than 0.5, 0.6.-1.5, and greater than 1.5 solar mass, respectively.

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