Haze Particles and Condensation in Pluto's Atmosphere Explored through Microphysical Modeling

Abstract:

To explore scenarios involving condensation in Pluto's atmosphere, a 1-D microphysics model based on the Community Aerosol and Radiation Model for Atmospheres (CARMA) has been developed. CARMA has been used successfully many times to explore the vertical distribution, size, shape, and composition of particles in Titan's atmosphere, and in particular, to predict the appearance of methane condensate layers which were observed at the Huygens' landing site. Physical processes in CARMA include nucleation, condensation, evaporation, sedimentation, and coagulation. In Pluto's atmosphere, most of the condensation would require the presence of a troposphere with at least a few kilometers vertical extent. However, if photochemical production proceeds similarly to the case of Titan's atmosphere, there are possibilities for condensation at higher altitudes as well. A number of sensitivity tests will be presented, including variations in the abundance, size, and shape of haze particles; evaluating the onset of homogeneous methane nucleation; exploring the size distribution of the resulting methane ice particles; and the effects of condensation of other photochemically produced trace species as well.