Stellar physics · L ≈ (M)^3.5 (solar units)

Mass–Luminosity Relation

The steep relation between a main-sequence star's mass and its luminosity: a star twice the Sun's mass shines roughly eleven times as bright. An approximation (exponent ~3.5) valid across the middle main sequence.

Mass (M☉)

Luminosity11.314L☉

Formula: L ≈ (M)^3.5 (solar units)

Worked example

With the default inputs, mass–luminosity relation evaluates to 11.314 L☉ — 2 M☉ → ~11 L☉. The validator recomputes this against the known value on every build, so the formula is checked, not asserted.

Highlights

›2 M☉ → ~11 L☉

The Hertzsprung–Russell Diagram

Knowledge connections

Associated withThe Hertzsprung–Russell Diagram

Sources

Facts on this topic will be cited from these primary and reference sources.

NASANational Aeronautics and Space Administration
Mission data, planetary science, space telescopes, and public-domain imagery.
Most NASA-produced imagery is in the public domain; individual items are checked for usage terms before publication.

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Mass–Luminosity Relation

Worked example

Highlights

The physics behind it

Knowledge connections

Sources

Mass–Luminosity Relation

Worked example

Highlights

The physics behind it

Knowledge connections

Sources