TY - JOUR
T1 - Saturn's satellites
T2 - Nuar-infrared spectrophotometry (0.6-2.5 μm) of the leading and trailing sides and compositional implications
AU - Clark, Roger N.
AU - Brown, Robert H.
AU - Owensby, Pamela D.
AU - Steele, Alex
N1 - Funding Information:
This research was supported by NASA Grants NSG 7323, NSG 7312, and NAGW 115. This is Planetary Geosciences Division publication No. 386. The majority of this research was completed while the senior author was at the Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii.
Funding Information:
1 Visiting Astronomer at the Infrared Telescope Facility which is operated by the University of Hawaii under contract to the National Aeronautics and Space Administration.
PY - 1984/5
Y1 - 1984/5
N2 - Near-infrared spectra, 0.65-2.5 μm, are presented for Tethys, Dione, Rhea, Iapetus, and Hyperion. Water ice absorptions at 2.0, 1.5, and 1.25 μm are seen in the spectra of all five objects (except the 1.25-μm band was not detected in spectra of Hyperion) and the weak 1.04-μm ice absorption is detected on the leading and trailing sides of Rhea, and the trailing side of Dione. Upper limits to the 1.04-μm ice band depth are <0.3% for the leading side of Dione; <0.7% for the leading side of Iapetus, and the trailing side of Tethys; <1% on the trailing side of Iapetus; and <5% on the leading side of Tethys. The leading-trailing side 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 determined for the amount of particulates, trapped gases, and amonium hydroxide on the surface. The surfaces of Saturn's satellites (except the dark side of Iapetus) are nearly pure water ice, with probably less than about 1 wt% particulate minerals. The ice could be clathrates with as much as a few weight percent trapped gases. The upper limit of amonium hydroxide depends on the spectral data precision and varies from ∼ 1 wt% NH3 for the leading side of Rhea to ∼ 10 wt% NH3 for Dione.
AB - Near-infrared spectra, 0.65-2.5 μm, are presented for Tethys, Dione, Rhea, Iapetus, and Hyperion. Water ice absorptions at 2.0, 1.5, and 1.25 μm are seen in the spectra of all five objects (except the 1.25-μm band was not detected in spectra of Hyperion) and the weak 1.04-μm ice absorption is detected on the leading and trailing sides of Rhea, and the trailing side of Dione. Upper limits to the 1.04-μm ice band depth are <0.3% for the leading side of Dione; <0.7% for the leading side of Iapetus, and the trailing side of Tethys; <1% on the trailing side of Iapetus; and <5% on the leading side of Tethys. The leading-trailing side 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 determined for the amount of particulates, trapped gases, and amonium hydroxide on the surface. The surfaces of Saturn's satellites (except the dark side of Iapetus) are nearly pure water ice, with probably less than about 1 wt% particulate minerals. The ice could be clathrates with as much as a few weight percent trapped gases. The upper limit of amonium hydroxide depends on the spectral data precision and varies from ∼ 1 wt% NH3 for the leading side of Rhea to ∼ 10 wt% NH3 for Dione.
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U2 - 10.1016/0019-1035(84)90043-5
DO - 10.1016/0019-1035(84)90043-5
M3 - Article
AN - SCOPUS:0001024824
SN - 0019-1035
VL - 58
SP - 265
EP - 281
JO - Icarus
JF - Icarus
IS - 2
ER -