Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.7205d&link_type=abstract
American Astronomical Society, DPS meeting #38, #72.05; Bulletin of the American Astronomical Society, Vol. 38, p.629
Other
Scientific paper
Surface compositions among the icy Saturnian satellites range from nearly pure water ice at Mimas and Tethys to dark, nitrile-laced compounds at Phoebe and Dione. New measurements from the Cassini Visual and Infrared Mapping Spectrometer (VIMS) coupled with laboratory measurements of relevant compounds at cryogenic temperatures, are beginning to reveal some of the subtle variations in compounds on these worlds. By comparing spectral observations for each of these moons to the others, inferences may be drawn which help to reveal their varying formation histories. Spectral modeling of Tethys observations, for example, indicates a surface dominated by water ice with only small contributions by other materials such as carbon dioxide or amorphous carbon; yet, requires an unusual mixture of grain sizes ranging from less than ten microns to as much as 2.5 millimeters in diameter. At the other extreme, Phoebe has been shown to exhibit much clearer evidence (cf. Clark et al., 2005) for a host of compounds, including iron-bearing materials, carbon dioxide, nitriles, and organics. Comparison of Cassini VIMS spectra of Phoebe, Dione, and Hyperion indicate many of the same spectral features. Mapping of these spectral features using automated feature extraction algorithms, cryogenic laboratory reflectance measurements, and standard Hapke reflectance models allows insights into the nature and distribution of these materials on the icy Saturnian satellites. In addition, this exercise allows examination of the methods and suggests ways in which the models might be improved. These include improved formulations of phase and scattering functions, as well as laboratory investigations of both pure compounds and mixtures.
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