Stellar physics · L = 4π R² σ T⁴
Stellar Luminosity (Stefan–Boltzmann)
A star's total power output, from its radius and surface temperature by the Stefan–Boltzmann law. Doubling the temperature raises luminosity sixteenfold.
Luminosity1L☉
Formula: L = 4π R² σ T⁴
Worked example
With the default inputs, stellar luminosity (stefan–boltzmann) evaluates to 1 L☉ — Sun (1 R☉, 5772 K) → 1 L☉. The validator recomputes this against the known value on every build, so the formula is checked, not asserted.
Highlights
- ›Sun: 1 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.