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Mass-Luminosity Relation

(model relating stellar mass and luminosity)

The Mass-Luminosity Relation is an equation relating a star's mass with its Luminosity.

 L         M
————— = ( ————— )a
 LSun      MSun

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.


Referenced by:
Initial Mass Function (IMF)
Mass-Radius Relation
Stellar Radius Determination