State and explain stefan's boltzman law of black body radiation.
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sources, 2013
3.1.1 Black-body radiation
Black-body radiation, also termed Planck’s law, determines the intensity of a radiation (Ie) at a wavelength (λ) from the temperature (T) of the emitter, if the latter is a perfect absorber and emitter (black body):
(F3.1.1)Ie(ν,T)=2hν3c−2/{exp[hν/k(B)T]−1}
where h and k(B) are Planck’s and Boltzmann’s constants respectively, and c is the speed of light, while ν = c/λ. Note that if the units of Ie are W m−2 nm−1 sr−1, then the unit of λ is nm. The “sr” denotes steradian, the unit of solid angle.
The Sun is very similar to a black body. Despite significant variations of the solar spectrum near the surface due to many atmospheric processes, especially clouds, total solar radiation in space has been found to be fairly constant. For example, at 645 km ASL, the daily average total solar radiation ranged from 1357 to 1362 W m−2, with an average of 1361 W m−2, from March 2003 to July 2012, according to satellite measurements in a recent mission, the Solar Radiation and Climate Experiment (SORCE) in the USA. Long-term satellite measurements in earlier missions.