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1.5 Basic Laws of Radiation 1.5.1 Stefan-Boltzmann Law
ОглавлениеThe Stefan-Boltzmann law is as the emissive power of a black body that is directly proportional to fourth power of its absolute temperature.
where Eb - Black body emissive power (W/m2)
σ - Stefan Boltzmann constant—5.67 × 10–8 W/m2 K4
T - Absolute temperature (K)