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E.H. Wilson, R.A. West (Caltech/Jet Propulsion Laboratory)
Titan’s stratospheric haze represents a significant source of opacity across much of Titan’s reflectance spectrum. These haze particles, created by the polymerization of complex hydrocarbons and nitriles and subsequent macromolecular nucleation, may act as nuclei for the condensation of clouds in the troposphere and provide opacity that may affect the distribution of chemical constituents and composition of clouds [1]. However, the characteristics of Titan haze are not entirely well understood. We use a chemically-based nucleation profile to investigate Titan’s haze properties, including particle size, structure, and refractive index, with a microphysical model [2]. A spherical shell radiative transfer model is applied to resulting haze profiles to examine haze opacity in the context of Voyager and ground-based observations of Titan’s albedo. Results will also be discussed in the framework of the Cassini-Huygens mission.
[1] E. H. Wilson and S. K. Atreya, J. Geophys. Res., 109, E06002, 2004. [2] A. J. Friedson, et al., Icarus, 158, 389-400, 2002.
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Bulletin of the American Astronomical Society, 36 #4
© 2004. The American Astronomical Soceity.