Stefan–Boltzmann law
Physical law on the emissive power of black body
Stefan–Boltzmann law
The Stefan–Boltzmann law, also known as Stefan's law, describes the intensity of the thermal radiation emitted by matter in terms of that matter's temperature. It is named for Josef Stefan, who empirically derived the relationship, and Ludwig Boltzmann who derived the law theoretically. For an ideal absorber/emitter or black body, the Stefan–Boltzmann law states that the total energy radiated per unit surface area per unit time (also known as the radiant exitance) is directly proportional to the fourth power of the black body's temperature, T {\displaystyle T} : M ∘ = σ T 4 . {\displaystyle M^{\circ }=\sigma \,T^{4}.} The constant of proportionality, σ {\displaystyle \sigma } , is called the Stefan–Boltzmann constant...
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