Saturn's satellites - Near-infrared spectrophotometry (0.65-2.5 microns) of the leading and trailing sides and compositional implications

Details Saturn's satellites - Near-infrared spectrophotometry (0.65-2.5 microns) of the leading and trailing sides and compositional implications Saturn's satellites - Near-infrared spectrophotometry (0.65-2.5 microns) of the leading and trailing sides and compositional implications

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...58..265c&link_type=abstract

(IAU, COSPAR, NASA, et al., Colloquium on Natural Satellites, 77th, Cornell University, Ithaca, NY, July 5-9, 1983) Icarus (ISSN

Computer Science

64

Abundance, Ice, Infrared Absorption, Infrared Spectra, Satellite Surfaces, Saturn Satellites, Ammonium Compounds, Chemical Composition, Near Infrared Radiation, Particulates, Spectral Reflectance, Saturn, Satellites, Infrared, Wavelengths, Spectrophotometry, Parameters, Composition, Spectra, Tethys, Dione, Rhea, Iapetus, Hyperion, Gases, Absorption, Surface, Comparisons, Charged Particles, Bombardment, Ice, Magnetosphere, Particles, Ammonia, Data, Observations

Scientific paper

Water ice absorptions at 2.0, 1.5, and 1.25 microns are noted in near-IR spectra of Tethys, Dione, Rhea, Iapetus, and Hyperion, and the weak 1.04-micron ice absorption, which is detected for Rhea and Dione, is studied to establish band depth upper limits. The leading-trailing side 1.04-micron ice band depth differences on Saturn's satellites are similar to those for the Galilean satellites, indicating possible surface modification by magnetospheric charged particle bombardment. Limits are obtained for the amounts of particulates, trapped gases, and ammonium hydroxide on the surface. With the exception of the dark side of Iapetus, the surfaces of all of Saturn's satellites are nearly pure ice water.

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