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.

Radius (R☉)Effective temperature (K)

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 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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Stellar Luminosity (Stefan–Boltzmann)

Worked example

Highlights

The physics behind it

Knowledge connections

Sources

Stellar Luminosity (Stefan–Boltzmann)

Worked example

Highlights

The physics behind it

Knowledge connections

Sources