Radiative-convective equilibrium models of Jupiter and Saturn

Details Radiative-convective equilibrium models of Jupiter and Saturn Radiative-convective equilibrium models of Jupiter and Saturn

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...59..336a&link_type=abstract

Icarus (ISSN 0019-1035), vol. 59, Sept. 1984, p. 336-366. NASA-supported research.

Computer Science

30

Atmospheric Heat Budget, Atmospheric Models, Jupiter Atmosphere, Saturn Atmosphere, Acetylene, Aerosols, Atmospheric Heating, Ethane, Methane, Opacity, Radiative Transfer, Planets, Jupiter, Saturn, Models, Equilibrium, Convection, Radiation, Stratosphere, Energy, Aerosols, Heating, Structure, Thermal Properties, Voyager Missions, Radio Occultations, Flux, Absorption, Emissions, Thermodynamics, Optical Properties, Opacity, Latitude, Calculations, Pressure, Temperature, Data

Scientific paper

Radiative-convective equilibrium models for Jupiter and Saturn have been produced in a study concentrating on the stratospheric energy balance and the possible role of aerosol heating. These models are compared directly with the thermal structure profiles obtained from Voyager radio occultation measurements. The method is based on a straightforward flux divergence formulation derived from earlier work. The balance between absorbed and emitted energies is computed iteratively at each level in the atmosphere, assuming local thermodynamic equilibrium and employing a standard treatment of opacities. Results for Jupiter indicate that a dust-free model furnishes a good mean thermal profile for the stratosphere when compared with the Voyager 1 radio occultation measurements. Observations of the equatorial region exhibit periodic vertical structure. The Saturn models are relatively simple and in good agreement with the Voyager 2 radio occultation temperature profiles at all levels. Aerosol heating played a minor role in Saturn's midlatitude stratospheric energy balance at the time of the Voyager 2 encounter.

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