Vertical Structure Of The Titan Atmosphere From Cassini Uvos Observations

Details Vertical Structure Of The Titan Atmosphere From Cassini Uvos Observations Vertical Structure Of The Titan Atmosphere From Cassini Uvos Observations

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.3608s&link_type=abstract

American Astronomical Society, DPS meeting #42, #36.08; Bulletin of the American Astronomical Society, Vol. 42, p.1066

Astronomy and Astrophysics

Astronomy

Scientific paper

The reduction and model analysis of Titan vertical atmospheric structure obtained from EUV/FUV stellar and solar occultations from Cassini UVIS experiment will be presented. Related atmospheric emission properties will also be described. The observations show both latitude and longitude dependencies in vertical structure of the hydrocarbon species. Dayside depletion of CH4 and higher order hydrocarbons is observed at altitudes above 880 km, allowing the establishment of limits on diffusion and production rates. Hydrocarbon mixing ratios show latitudinal dependencies of as much as a factor of 4. Higher order hydrocarbons including extinction by aerosols show scale heights larger than CH4 below the exobase, indicating that these species are showing the impact of forcing by chemical production and downward diffusion. The higher order hydrocarbons show density peaks in the 500 -- 700 km region. Aerosol mixing ratios decrease with decreasing altitude as do the higher order hydrocarbons down to 450 km where the distribution makes a sudden transition to constancy with the major species. The aerosols, as the end point of hydrocarbon physical chemistry, constitute the key component determining the state of the atmosphere.

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