The structure of the Uranian atmosphere - Constraints from the geometric albedo spectrum and H2 and CH4 line profiles

Details The structure of the Uranian atmosphere - Constraints from the geometric albedo spectrum and H2 and CH4 line profiles The structure of the Uranian atmosphere - Constraints from the geometric albedo spectrum and H2 and CH4 line profiles

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...65..406b&link_type=abstract

Icarus (ISSN 0019-1035), vol. 65, Feb.-Mar. 1986, p. 406-441. NASA-supported research.

Computer Science

66

Atmospheric Models, Hydrogen, Line Spectra, Methane, Uranus Atmosphere, Albedo, Fraunhofer Lines, Haze, Radiative Transfer, Stratosphere, Troposphere, Uranus, Atmosphere, Structure, Albedo, Spectra, Hydrogen, Troposphere, Methane, Analysis, Models, Haze, Pressure, Optical Properties, Depth, Aerosols, Infrared, Wavelengths, Theoretical Studies, Laboratory Studies, Comparisons

Scientific paper

Recent high quality spectral observations have allowed the derivation of constraints on the atmospheric structure of Uranus. The present analysis, which is based on the detailed modeling of a broadband geometric albedo spectrum and high resolution observations of the H2 4-0 quadrupole and 6818.9-A CH4 features, yields (1) a family of models which parameterize an upper tropospheric haze layer, (2) a lower, optically infinite cloud at a given pressure level, (3) the cloud-level methane molar fraction, and (4) the mean ortho/para ratio in the visible atmosphere. The single scattering albedo of atmospheric aerosols exhibits a steep darkening between 5890 and 6040 A.

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