Titan'S Haze Structure from Cassini ISS and UVIS Observations

Details Titan'S Haze Structure from Cassini ISS and UVIS Observations Titan'S Haze Structure from Cassini ISS and UVIS Observations

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.2202w&link_type=abstract

American Astronomical Society, DPS meeting #38, #22.02; Bulletin of the American Astronomical Society, Vol. 38, p.519

Astronomy and Astrophysics

Astronomy

1

Scientific paper

New observations by the Cassini Imaging Science Subsystem (ISS) and Ultraviolet Imaging Spectrograph (UVIS) are providing valuable information on Titan's haze. UVIS stellar occultations and ISS images show a prominent thin but distinct haze layer near 500 Km altitude at latitudes south of the polar vortex boundary near +55 degrees. At higher northern latitudes this layer dissipates but numerous layers can be seen between about 300 and 500 Km altitudes. These evolve on short time scales. Images of reflected sunlight in the ultraviolet are sensitive to the smallest particles and the highest altitudes. We also have measurements of intensity and polarization at continuum wavelengths and in three methane bands. Implications for particle properties and vertical haze structure from multiple-scattering analyses of these data will be discussed.

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