The Stefan-Boltzmann law describes the relationship between the temperature of a black body and the total energy radiated per unit surface area across all wavelengths per unit time (also known as the black body radiation). The law states that the power radiated per unit area \( j^* \) of a black body is proportional to the fourth power of its absolute temperature \( T \).
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The Stefan–Boltzmann law gives the thermal-radiation flux emitted by a surface as , where is its emissivity and is the Stefan–Boltzmann constant.