Physics
Scientific paper
Dec 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985esasp.241..109t&link_type=abstract
In ESA The Atmospheres of Saturn and Titan p 109-119 (SEE N86-28849 19-88)
Physics
2
Atmospheric Chemistry, Atmospheric Models, Nitrogen Hydrides, Satellite Atmospheres, Titan, Abundance, Chemical Composition, Cloud Physics, Oceans, Opacity, Troposphere
Scientific paper
Phase equilibria in the N2-CH4-C2H6-C3H8 system are modeled using an expression for activity coefficients in multicomponent systems. An accurate quantitative model of the behavior of this system is important to considerations of the ocean-atmosphere, atmosphere-cloud, and thermal equilibria in the troposphere of Titan. In the model, the interrelationship between the tropospheric gas phase CH4 abundance, the ocean composition, and temperature is well defined. Given two of these three (and the total pressure), the third variable is fixed. Given a surface inventory of any one component, the total ocean depth is also fixed. A Titan ocean seems likely, is of a single liquid phase, and is involved in a strong feedback couple with the tropospheric temperature through the thermal opacity of CH4. A large part of this opacity is contributed by the clouds, which are a liquid solution of 15 to 25 mol% N2 in CH4 below 16 km, a solid solution of 13 to 26 mol% N2 in CH4 above, and are present at a column density 0.7 gm sqcm.
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