The Mass-Luminosity Relation is an equation relating a star's mass with its Luminosity (L).
L M ————— = ( ————— )a LSun MSun
a = 3.5 is often applied to main-sequence stars. Stars close to the Eddington Luminosity have a close to 1. "a" depends upon whether the star is the right size for significant convection.
Initial Mass Function (IMF)
Stellar Radius Determination