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P eσA T 4 T 04.
Stefan boltzmann equation. 4 Here is the emissivity of the object A s is the surface area and σ is the Stefan-Boltzmann constant. Where σ Stefans constant 567 10 -8 W m -2 K -4 E Radiant Energy. Using the Stephens Boltzmann law calculate the initial value of net power emitted by the body.
Where σ is a fundamental physical constant called the StefanBoltzmann constant which is equal to 5669710-8 Wm 2 K 4. This law is therefore called the Stefan-Boltzmann Law. Then P T4 watts m2 3 Radiative transfer of heat between two objects occurs when they are not at the same temperature.
Here is the Stefan-Boltzmann equation applied to the Sun. Where E total flux ε effective emissivity a value between 0 and 1 σ is a constant and T. This integration results in the Stefan-Boltzmann law which states6 that for an object of temperature T the radiated power P will be P rad σA sT 4.
The formula used to determine at what wavelength the power peaks at is Wiens LawThe Stefan-Boltzmann Law explains how much power the Sun gives off given its temperature or allows. Equation 2 can be easily modified to accommodate emission from a grey ie. Sigma is the Stefan-Boltzmann constant and it has a value of 567 X 10-8 Wm2K4.
For hot objects other than ideal radiators the law is expressed in the form. This works for any star. Rearranging the equation above.
The question that this article tries to help readers understand is the origin and use of the emissivity term in the Stefan-Boltzmann equation. It helps to resolve the unknown quantity between radiation emitted by the body temperature and the surface area. If E is the radiant heat energy emitted.
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