MathLiveStefan-Boltzmann law
Gives the total power per unit area radiated by an ideal black body, which grows with the fourth power of its absolute temperature. It is used to estimate the radiated energy of stars, planets, and other hot objects.
M_{\mathrm{b}} = \sigma T^4What the symbols mean
| radiant exitance (emissive power) of a black body, in \mathrm{W\,m^{-2}} | |
| Stefan-Boltzmann constant, approximately 5.67 \times 10^{-8} \mathrm{W\,m^{-2}\,K^{-4}} | |
| thermodynamic temperature of the body, in kelvins |
About this formula
- FieldPhysics
- TopicThermodynamics and radiation
- LevelUniversity
- Also calledStefan's law, blackbody radiation power, black body emissive power, radiant exitance of black body, Stefan-Boltzmann equation
- SourceWikidata Q704747
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