In astrophysics, the mass–luminosity relation is an equation giving the relationship between a star's mass and its luminosity, first noted by Jakob Karl Ernst Halm.[1] The relationship is represented by the equation:
L
L
⊙
=
(
M
M
⊙
)
a
{\frac {L}{L_{{\odot }}}}=\left({\frac {M}{M_{{\odot }}}}\right)^{a}
where L⊙ and M⊙ are the luminosity and mass of the Sun and 1
