Stephen’s Law and Its Significance in Astrophysics
It is a fundamental law of physics that describes the intensity of thermal radiation emitted by matter in terms of its temperature. The law states that the total energy radiated per unit surface area of a black body across all wavelengths per unit time is directly proportional to the fourth power of the black body’s thermodynamic temperature.
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Mathematical form of Stephen’s law
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The formula for the Stephen’s law is:
L = AơT4
L = brightness of the star. Lightness in reality is a measure of total yield by a star. This rule is also called the Stefan Volzmann Rule.
Our objective is to understand the basic principle behind this rule, so we start from the empty slate.
Where P is the power radiated, A is the surface area of the black body, T is the temperature of the black body, and σ is the Stefan-Boltzmann constant, which has a value of 5.67×10−8W/m2K4.
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