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Session 42 - Solar Systems.
Display session, Tuesday, January 16
North Banquet Hall, Convention Center
The gas flux of the volatile icy components from the surface of 2060 Chiron is calculated in order to compare our model with observed relative molecular abundances in the coma. The model assumes a body containing dust, one major ice component (H_2O), and minor components of higher volatility. The mass and energy equations for the different volatiles are solved simultaneously with appropriate boundary conditions. The model includes inward and outward flowing gas within the body, escape of outward flowing gas from the body, depletion of less volatile ices in outer layers, recondensation of gas in deeper, cooler layers, and changing porosity as a result of sublimation. Results are presented from calculations which are able to explain recent observations of CO in the coma. Interpretation of these results leads to conclusions about the pore radius and the inhomogeneous structure of 2060 Chiron.
\hspace*0.3mmSupport from NASA Planetary Atmospheres Program, from the German Science Foundation, and from the SwRI Internal Research Program is acknowledged.
