A new spherical model for computing the radiation field available for photolysis and heating at twilight

Details A new spherical model for computing the radiation field available for photolysis and heating at twilight A new spherical model for computing the radiation field available for photolysis and heating at twilight

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991p%26ss...39..671d&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 39, May 1991, p. 671-683.

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Computation

103

Atmospheric Chemistry, Atmospheric Heating, Atmospheric Models, Atmospheric Radiation, Photolysis, Night Sky, Photodissociation, Radiative Transfer, Reaction Kinetics

Scientific paper

Accurate computation of atmospheric photodissociation and heating rates is needed in photochemical models. These quantities are proportional to the mean intensity of the solar radiation penetrating to various levels in the atmosphere. For large solar zenith angles a solution of the radiative transfer equation valid for a spherical atmosphere is required in order to obtain accurate values of the mean intensity. Such a solution based on a perturbation technique combined with the discrete ordinate method is presented. Mean intensity calculations are carried out for various solar zenith angles. These results are compared with calculations from a plane parallel radiative transfer model in order to assess the importance of using correct geometry around sunrise and sunset. This comparison shows, in agreement with previous investigations, that for solar zenith angles less than 90 deg adequate solutions are obtained for plane parallel geometry as long as spherical geometry is used to compute the direct beam attenuation; but for solar zenith angles greater than 90 deg this pseudospherical plane parallel approximation overstimates the mean intensity.

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