Saturn's satellites - Near-infrared spectrophotometry (0.65-2.5 microns) of the leading and trailing sides and compositional implications
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 ba...
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Veröffentlicht in: | Icarus (New York, N.Y. 1962) N.Y. 1962), 1984-05, Vol.58 (2), p.265-281 |
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creator | Steele, A. Clark, R. N. Brown, R. H. Owensby, P. D. |
description | 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. |
doi_str_mv | 10.1016/0019-1035(84)90043-5 |
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source | Elsevier ScienceDirect Journals; NASA Technical Reports Server |
subjects | Astronomy Earth, ocean, space Exact sciences and technology Planets, their satellites and rings. Asteroids Saturn Solar system |
title | Saturn's satellites - Near-infrared spectrophotometry (0.65-2.5 microns) of the leading and trailing sides and compositional implications |
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