A novel methodology for radiative transfer in a planetary atmosphere. I - The functions a exponent M and B exponent M of anisotropic scattering

Details A novel methodology for radiative transfer in a planetary atmosphere. I - The functions a exponent M and B exponent M of anisotropic scattering A novel methodology for radiative transfer in a planetary atmosphere. I - The functions a exponent M and B exponent M of anisotropic scattering

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977ap%26ss..47..195f&link_type=abstract

Astrophysics and Space Science, vol. 47, Mar. 1977, p. 195-216

Physics

Optics

4

Atmospheric Radiation, Planetary Atmospheres, Radiative Transfer, Atmospheric Optics, Boundary Value Problems, Radiation Distribution

Scientific paper

The original problem of anisotropic scattering in an atmosphere illuminated by a unidirectional source is replaced by an analogous formulation where the incident light is omnidirectional. A radiative-transfer equation for the omnidirectional case is obtained in which the direction of illumination plays no role and the source-function analog, Sobolev's (1972) source function Phi exponent m, contains only a single integral term. For radiation incident on the top or the bottom of the atmosphere, this equation involves the functions b exponent m and h exponent m, respectively, with m corresponding to the order of the harmonic component of the scattered radiation field; these two functions are shown to be only one through some simple reciprocity relations. The transfer problem is then reformulated for the function a exponent m, in which case the source-function analog (Sobolev's function D exponent m) involves incident direction.

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