Brightness temperature
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Brightness temperature is the temperature a black body in thermal equilibrium with its surroundings would have to be to duplicate the observed intensity of a grey body object at a frequency . This concept is extensively used in radio astronomy and planetary science.
For a black body, Planck's law gives[1] :
where
(the Intensity or Brightness) is the amount of energy per unit surface per unit time per unit solid angle emitted in the frequency range between and , is the temperature of the black body, is Planck's constant, is frequency, is the speed of light and is Boltzmann's constant.
For a grey body the spectral radiance is a portion of the black body radiance, determined by the emissivity . That makes the reciprocal of the brightness temperature:
At low frequency and high temperatures, when , we can use the Rayleigh–Jeans law:
so that the brightness temperature can be simply written as:
In general, the brightness temperature is a function of , and only in the case of blackbody radiation is it the same at all frequencies. The brightness temperature can be used to calculate the spectral index of a body, in the case of non-thermal radiation.
[edit] See also
Compare with color temperature and effective temperature.
[edit] References
- ^ Rybicki, George B., Lightman, Alan P., (2004) Radiative Processes in Astrophysics, ISBN 978-0-471-82759-7
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