Mass–luminosity relation

In astrophysics, the mass–luminosity relation is an equation giving the relationship between a star's mass and its luminosity. The relationship is represented by the equation:

where L_⊙ and M_⊙ are the luminosity and mass of the Sun and 1 < a < 6. The value a = 3.5 is commonly used for main-sequence stars. This equation and the usual value of a = 3.5 only applies to main-sequence stars with masses 2M_⊙ < M < 20M_⊙ and does not apply to red giants or white dwarfs. As a star approaches the Eddington Luminosity then a = 1.

单词	Mass luminosity relation
释义	Mass luminosity relation 英语百科 Mass–luminosity relation In astrophysics, the mass–luminosity relation is an equation giving the relationship between a star's mass and its luminosity. The relationship is represented by the equation: where L_⊙ and M_⊙ are the luminosity and mass of the Sun and 1 < a < 6. The value a = 3.5 is commonly used for main-sequence stars. This equation and the usual value of a = 3.5 only applies to main-sequence stars with masses 2M_⊙ < M < 20M_⊙ and does not apply to red giants or white dwarfs. As a star approaches the Eddington Luminosity then a = 1.
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Mass luminosity relation

Mass–luminosity relation