Radiative forcing of the Venus mesosphere. I - Solar fluxes and heating rates

Details Radiative forcing of the Venus mesosphere. I - Solar fluxes and heating rates Radiative forcing of the Venus mesosphere. I - Solar fluxes and heating rates

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...67..484c&link_type=abstract

Icarus (ISSN 0019-1035), vol. 67, Sept. 1986, p. 484-514.

Physics

Optics

54

Astronomical Models, Atmospheric Heating, Mesosphere, Radiative Heat Transfer, Solar Planetary Interactions, Venus Atmosphere, Aerosols, Atmospheric Attenuation, Atmospheric Composition, Atmospheric Optics, Solar Flux

Scientific paper

Most of the solar energy absorbed by Venus is deposited in the atmosphere, at levels more than 60 km above the surface. This unusual flux distribution should have important consequences for the thermal structure and dynamical state of that atmosphere. A radiative transfer model was used to derive the structure and amplitude of the solar fluxes and heating rates in the Venus mesosphere (60 - 100 km). This model accounts for all sources of extinction known to be important there, including absorption and scattering by CO2, H2O, SO2, H2SO4 aerosols and an unidentified UV absorber. The distributions of these substances in the model atmosphere were constrained by a broad range of spacecraft and ground-based observations.

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