The Diverse Surface Compositions of the Galilean Satellites

Details The Diverse Surface Compositions of the Galilean Satellites The Diverse Surface Compositions of the Galilean Satellites

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002assl..278....9c&link_type=abstract

Solar System Remote Sensing, p. 9

Computer Science

Galilean Satellites, Planetary Surfaces, Planetary Composition, Spectral Reflectance, Planetary Geology, Radiolysis, Remote Sensing

Scientific paper

The galilean satellites represent a diverse collection, ranging from the volcanic moon Io, with a surface that is changing yearly, to Callisto, with a dark, ancient surface overlying ice. The composition of these surfaces are also quite different due to a variety of processes and influences, including tidal heating, radiolysis, gardening, a magnetic field (Ganymede), and meteoritic infall. Io's surface contains large quantities of sulfur dioxide (SO2) and colorful sulfur allotropes, both originating in plumes and flows from the tidally driven volcanoes. A broad, 1-micron band is found at high latitudes and may be due to absorption by long-chain sulfur polymers produced by SO2 radiolysis, although iron and iron sulfide compounds are candidates. An unidentified 3.15 micron absorber is equatorially distributed while a 4.62 micron band, perhaps due to a sulfate compound, exhibits a non-uniform distribution. Hot spots are generally dark, and some exhibit negative reflectance slopes (i.e., blue). The composition of these lavas has not been established spectroscopically, but the high temperatures of some volcanoes suggest ultramafic silicates or perhaps more refractory material such as oxides.

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