Mass-luminosity relation of intermediate-mass stars

Abstract

The mass–luminosity relation (MLR) for intermediate-mass stars is based on data on detached double-lined eclipsing binaries. However, there is a notable difference between the parameters of B0V–G0V components of eclipsing binaries and those of single stars. Single early-type stars are rapid rotators, whereas tidal forces produce synchronous rotation in close binaries and all such pairs are synchronized, so components of close binaries rotate more slowly. As is well known, stellar rotation changes stellar evolution and the global parameters of a star.