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Calculations of the total radiation emerging from planetary atmospheres optically thicker than those of the earth. For Rayleigh scattering and Lambert reflectivity, the flux is determined for a wide range of solar elevations, ground reflectivities, and optical depths. For very large surface reflectivities there is more radiation downward onto a planet at the bottom of a thick atmosphere than is received at the top because the radiation that does penetrate undergoes multiple reflection. The total radiation absorbed by the surface plus the corresponding diffuse upward radiation always equals the input flow. Bond albedo is determined by numericaly integration. It approaches the value of the ground reflectivity as optical thickness approaches zero, and approaches 1 as it becomes very large. (Author).
Theoretically derived values of the directional intensity of radiation emerging from both the top and the bottom of a Rayleigh scattering atmosphere are presented graphically. The model assumes a plane-parallel atmosphere illuminated by the sun, with either a completely absorbing planetary surface or Lambert ground reflection. By using Mullikin's and Sekera's recent modification of Chandrasekhar's radiative-transfer theory, the intensities were obtained for much larger values of the optical thickness of the atmosphere than was previously possible. These intensities are given for a wide range of optical thicknesses, solar zenith angles, and directions of emergence. (Author).
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Rayleigh scattering intensities in the altitude range of 80-300 km are calculated using the concentrations of the principal atmospheric constituents N2, O2 and O. The polarizability of the oxygen atom is calculated from atomic oscillator strengths and normal and slant optical thicknesses are calculated as a function of altitude. (Author).
The problem of radiative transfer in plane-parallel, perfectly scattering atmosphere is described. Chandrasekhar's solution applicable to atmospheres of small and moderate optical thickness is outlined. His solution reduces the problem to that of determining the X-, Y-, K-, and L-functions, the scattering functions. Mullikin has extended this method of solution to atmospheres of large optical thickness. Sekera and Kahle have used Mullikin's method of solution of calculating the emergent radiation from plane-parallel Rayleigh-scattering atmospheres of large optical thickness. Their numerical results are reproduced here in the Appendix, as tables of scattering functions. The numerical method for determining the intensity and polarization of the radiation emerging from the top and bottom of atmospheres is given, and suggestions for additional uses of the tables are made. Finally, a few examples of representative calculations are presented. (Author).
The industrial and military applications of atomic energy have stimulated much mathematical research in neutron transport theory. The possibility of controlled thermonuclear processes has similarly focussed attention upon plasmas, sometimes called the "fourth state of matter". Independently, many classical aspects of kinetic theory and radiative transfer theory have been studied both because of their basic mathematical interest and of their physical applications to areas such as upper-atmosphere meteorology - introduction.