A saturation model of the atmosphere of Uranus

Details A saturation model of the atmosphere of Uranus A saturation model of the atmosphere of Uranus

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977icar...31...97d&link_type=abstract

Icarus, vol. 31, May 1977, p. 97-109.

Computer Science

10

Atmospheric Composition, Atmospheric Models, Planetary Atmospheres, Uranus (Planet), Abundance, Albedo, H Lines, Hydrogen, Infrared Spectra, Methane, Molecular Spectra, Solar Heating

Scientific paper

A model of the atmospheric structure of Uranus is presented which differs from previous types of models in two important respects: (1) the CH4/H2 ratio is sufficiently large that CH4 is saturated to large depths in the Uranian atmosphere and (2) the internal energy flux is small compared with that due to solar heating. Because of the small internal flux, the thermal flux decreases rapidly with depth and the atmosphere is radiative to large optical depths. A CH4 droplet cloud forms where the atmosphere finally becomes convective due to the internal flux. The model is shown to be in reasonable agreement with published observations of the H2 quadrupole 3-0 and 4-0 bands, the visible (4000-6000 A) CH4 bands, and the infrared emission spectrum.

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