This relationship is called the Stefan–Boltzmann law in honor of its late19th-century discoverers.
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Equation (1-9) is called the Stefan-Boltzmann law of thermal radiation, and it applies only to blackbodies.
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The wavelength at which the radiation is strongest is given by Wien's displacement law, and the overall power emitted per unit area is given by the Stefan–Boltzmann law.
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In 1879, Jožef Stefan observed that the total radiant flux from a blackbody is proportional to the fourth power of its temperature and stated the Stefan–Boltzmann law.
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Five years later, Austrian physicist Ludwig Boltzman derived the same equation and is now known as the Stefan-Boltzman law. If we assume a spherical star with radius R, then the luminosity of such a star is