Tholins in the Upper Atmosphere of Titan

Details Tholins in the Upper Atmosphere of Titan Tholins in the Upper Atmosphere of Titan

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.6108y&link_type=abstract

American Astronomical Society, DPS meeting #42, #61.08; Bulletin of the American Astronomical Society, Vol. 42, p.1089

Astronomy and Astrophysics

Astronomy

Scientific paper

The Ultraviolet Imaging Spectrograph Subsystem (UVIS) onboard the Cassini spacecraft is the only experiment with capability of measuring the tholin distribution from 1000 km altitude to 300 km along with the high order hydrocarbons. It is clear that tholins form at high altitude in the ionosphere, and precipitate downward, resulting in the manifestation of a large scale-height, completely different from a diffusively separated atmosphere (Liang et al. 2007). Preliminary analysis of Cassini T0 and TA encounters shows that production of aerosols is severely depleted in the polar region where solar scattering cannot be detected above 675 km, while in the sub-solar atmosphere aerosol scattering is measured to 1425 km altitude. In addition to extinction, there is valuable complementary information to be extracted from an analysis of the UV light scattered by tholins. The optical properties of tholins are studied using a multi-sphere method, and the results are used in a radiative code to simulate the UVIS observations.

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