How it works
Luminosity scales with the fourth power of temperature: a star twice as hot as the Sun with the same size is 16 times more luminous. Effective temperature is defined so that this law holds exactly.
Variables
L— luminosityσ— Stefan–Boltzmann constant 5.670374 × 10⁻⁸ W m⁻² K⁻⁴R, T— stellar radius and effective temperature
Assumptions and limits
- Star radiates as a black body at its effective temperature
- Spherical star
For education only. These models are simplified and are not suitable for spacecraft navigation or safety-critical engineering. See our scientific accuracy policy.