Brightness temperature | Wikipedia audio article
Channel: wikipedia tts
Date: 2019-06-17

This is an audio version of the Wikipedia Article:
https://en.wikipedia.org/wiki/Brightness_temperature


00:05:48 Calculating by frequency
00:08:16 Calculating by wavelength



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SUMMARY
=======
Brightness temperature or radiance 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 
  
    
      
        ν
      
    
    {\displaystyle \nu }
  .
This concept is used in radio astronomy, planetary science and materials science. 
The brightness temperature of a surface is typically determined by an optical measurement, for example using a pyrometer, with the intention of determining the real temperature. As detailed below, the real temperature of a surface can in some cases be calculated by dividing the brightness temperature by the emissivity of the surface. Since the emissivity is a value between 0 and 1, the real temperature will be greater than or equal to the brightness temperature. At high frequencies (short wavelengths) and low temperatures, the conversion must proceed through Planck's law.
The brightness temperature is not a temperature as ordinarily understood. It characterizes radiation, and depending on the mechanism of radiation can differ considerably from the physical temperature of a radiating body (though it is theoretically possible to construct a device which will heat up by a source of radiation with some brightness temperature to the actual temperature equal to brightness temperature). Nonthermal sources can have very high brightness temperatures. In pulsars the brightness temperature can reach 1026 K. For the radiation of a typical helium–neon laser with a power of 60 mW and a coherence length of 20 cm, focused in a spot with a diameter of 10 µm, the brightness temperature will be nearly 14×109 K.
For a black body, Planck's law gives:

  
    
      
        
          I
          
            ν
          
        
        =
        
          
            
              2
              h
              
                ν
                
                  3
                
              
            
            
              c
              
                2
              
            
          
        
        
          
            1
            
              
                e
                
                  
                    
                      h
                      ν
                    
                    
                      k
                      T
                    
                  
                
              
              −
              1
            
          
        
      
    
    {\displaystyle I_{\nu }={\frac {2h\nu ^{3}}{c^{2}}}{\frac {1}{e^{\frac {h\nu }{kT}}-1}}}
  where

  
    
      
        
          I
          
            ν
          
        
      
    
    {\displaystyle I_{\nu }}
   (the Intensity or Brightness) is the amount of energy emitted per unit surface area per unit time per unit solid angle and in the frequency range between 
  
    
      
        ν
      
    
    {\displaystyle \nu }
   and 
  
    
      
        ν
        +
        d
        ν
      
    
    {\displaystyle \nu +d\nu }
  ; 
  
    
      
        T
      
    
    {\displaystyle T}
   is the temperature of the black body; 
  
    
      
        h
      
    
    {\displaystyle h}
   is Planck's constant; 
  
    
      
        ν
      
    
    {\displaystyle \nu }
   is frequency; 
  
    
      
        c
      
    
    {\displaystyle c}
   is the speed of light; and 
  
    
      
        k
      
    
    {\displaystyle k}
   is Boltzmann's constant.
For a grey body the  spectral radiance is a portion of the black body radiance, determined by the emissivity 
  
    
      
     ...