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.
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 physics behind it
Knowledge connections
- Associated withThe Hertzsprung–Russell Diagram
Sources
The primary and reference sources this topic draws on.
- 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.