The Surface Properties of Titan as Revealed by Cassini VIMS

Details The Surface Properties of Titan as Revealed by Cassini VIMS The Surface Properties of Titan as Revealed by Cassini VIMS

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusm.p21c..01b&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #P21C-01

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5764 Surfaces, 6020 Ice, 6062 Satellites, 6280 Saturnian Satellites

Scientific paper

The Cassini Visual Infrared Mapping Spectrometer is an instrument that returns data between 0.34 and 5.1 microns. Spatial resolution can be as high as 0.25 mradians in the 1-5 micron range and 0.17 mradians in the visible. By the end of May 2005 the Cassini spacecraft will have accomplished 5 close, targeted flybys of Titan, ranging in distances (at closest approach) from 1025 to 4009 km. The VIMS instrument is uniquely suited to studying the surface of Titan because its thick, opaque nitrogen-methane atmosphere exhibits clarity at selected "windows" that are well-distributed throughout the near infrared. The spectral reflectance at these windows has been studied to derive the surface properties of the satellite. A simple empirical model has employed to remove the haze, which adds substantial opacity even in the windows. The surface scattering properties have been fit to a macroscopic roughness model, and to a Henyey-Greenstein equation to derive the single particle phase function. Many areas of Titan have scattering properties - and presumably surface properties - similar to the other icy satellites of Saturn. The over-all shape of Titan's spectrum through the atmospheric windows is consistent with a mixture of water-ice and organics (tholins), although this simple picture cannpt explain some details. Work funded by the National Aeronautics and Space Administration.

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