The Mass-Luminosity Relation is an equation
relating a star's mass with its Luminosity.
————— = ( ————— )a
a = 3.5 is often used for 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.
eclipsing binaries and Parallax measurements
help confirm the relation.
Initial Mass Function (IMF)
Stellar Radius Determination