A Fully-Kinetic Approach to Modeling Titan's Upper Atmosphere

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Possessing an appreciable atmosphere, Titan is a significant source of material in the Saturnian magnetosphere. This makes it an important object for understanding the nature of magnetospheric ions and the distribution and escape of neutral components from its atmosphere.
The quantitative description of the escape is complicated by Titan's interaction with ambient magnetospheric plasma. Together heating by absorption of solar radiation, impact ionization and sputtering by magnetospheric electrons and ions can increase the total escape rate. In addition, the decreasing efficiency of intermolecular collisions around exbase altitudes ( 4310 km) raises the question of the physically correct description of the gas flow regarding the normally used fluid approach, especially for light species. For this reason, we have begun looking at the conditions in Titan's upper atmosphere beginning somewhat below the exobase using a physical model that accounts for the kinetic nature of processes occurring in Titan's atmosphere.
Presented in this paper, a kinetic model has been developed for simulation of escape of N2 and CH4 and can be used to study the distributions of neutral species throughout the Titan's upper atmosphere and exosphere. The model is compared with fluid results obtained by other authors and available observational data.

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