Stefan–Boltzmann constant and thermal emission

stefanBoltzmann is the constant in the Stefan–Boltzmann law, which gives blackbody emitted power per area as proportional to the fourth power of absolute temperature.

Use

Estimate ideal radiative power with σT⁴, often adjusted by emissivity. Compare boltzmann and secondRadiation for related blackbody constants.

Caveats

Real surfaces are not perfect blackbodies. Temperature must be in kelvin and the fourth power matters; use pow with care and multiply for area and emissivity.