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Stefan–Boltzmann law
The Stefan–Boltzmann law describes the power radiated from a black body in terms of its temperature. Specifically, the Stefan–Boltzmann law states that the total energy radiated per unit surface area of a black body across all wavelengths per unit time (also known as the black-body radiant exitance or emissive power), j {\displaystyle j^{\star }} , is directly proportional to the fourth power of the black body's thermodynamic temperature T: MORE
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