M/L relation of intermediate-mass stars

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. In this work we collect data on fundamental parameters of stars with masses m>1.5m_{sun}_. They are components of binaries with P>15d and consequently are not synchronized with the orbital periods and presumably are rapid rotators.