Cassini VIMS Measurements of Titan's Surface Albedo; Preliminary Results.

Details Cassini VIMS Measurements of Titan's Surface Albedo; Preliminary Results. Cassini VIMS Measurements of Titan's Surface Albedo; Preliminary Results.

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21743503j&link_type=abstract

American Astronomical Society, AAS Meeting #217, #435.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

One of the main scientific objectives of the Cassini mission is to determine the surface composition and its distribution on Titan. Towards this objective, the Cassini spacecraft possesses an instrument called the Visual and Infrared Mapping Spectrometer (VIMS), which is designed to measure reflected and emitted UV to near-IR spectra from the atmospheres and surfaces of Saturn and its moons. We use a discrete ordinates radiative transfer model of Titan's atmosphere that can separately determine the surface albedo and scattering characteristics of the atmosphere. The scattering characteristics of the tropical atmosphere were derived from the Descent Imager-Spectral Radiometer (DISR) onboard the Huygens probe during its decent. We limited our study to the tropical region of Titan. The albedo of Titan's surface can only be determined through atmospheric windows that peer through Titan's thick atmosphere. For this reason we are able to determine only the albedo at 1.08 microns, 1.28 microns, and 1.58 microns. Knowledge of the albedo of Titan's surface is a crucial step in determining the composition of the surface. We present here preliminary results of several regions near the Huygens landing site on Titan where the surface albedo has been accurately determined.

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