Physics
Scientific paper
Apr 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999icar..138..268m&link_type=abstract
Icarus, Volume 138, Issue Icarus, pp. 268-286.
Physics
35
Scientific paper
Application of a radiative-convective equilibrium model to the thermal structure of Uranus'atmosphere evaluates the role of hazes in the planet's stratospheric energy budget and places a lower limit on the internal energy flux. The model is constrained by Voyager and post-Voyager observations of the vertical aerosol and radiatively active gas profiles. Our baseline model generally reproduces the observed tropospheric and stratospheric temperature profile. However, as in past studies, the model stratosphere from about 10^-3 to 10^-1 bar is too cold. We find that the observed stratospheric hazes do not warm this region appreciably and that any postulated hazes capable of warming the stratosphere sufficiently are inconsistent with Voyager and ground-based constraints. We explore the roles played by the stratospheric methane abundance, the H_2 pressure-induced opacity, photochemical hazes, and C_2H_2 and C_2H_6 in controlling the temperature structure in this region. Assuming a vertical methane abundance profile consistent with that found by the Voyager UVS occultation observations, the model upper stratosphere, from 10 to 100mubar, is also too cold. Radiation in the 7.8-μm band from a small abundance of hot methane in the lower thermosphere absorbed in this region can warm the atmosphere and bring models into closer agreement with observations. Finally, we find that internal heat fluxes ⋦60 erg cm^-2 sec^-1 are inconsistent with the observed tropospheric temperature profile.
Marley Mark S.
McKay Christopher P.
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