Geologic processes on the Galilean satellite Callisto: Galileo SSI results, open questions, and requirements for camera data in a future mission to Jupiter

Details Geologic processes on the Galilean satellite Callisto: Galileo SSI results, open questions, and requirements for camera data in a future mission to Jupiter Geologic processes on the Galilean satellite Callisto: Galileo SSI results, open questions, and requirements for camera data in a future mission to Jupiter

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..858w&link_type=abstract

European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a

Mathematics

Logic

Scientific paper

The second-largest satellite of Jupiter, Callisto, is characterized by a unique surface geology dominated by impact and erosional processes [1][2]. Tectonic features occur but are much less pervasive than on Callisto's inner neighbour Ganymede [1][2][3]. It remains still an unsolved question if cryovolcanism was ever active in Callisto's early history [2][3][4][5]. One common feature of the two largest Galilean satellites Callisto and Ganymede is the strong similarity in impact crater forms which implies a similar sub-surface structure [1][6][7]. Since Callisto's surface was the least imaged one by the Galileo SSI camera, the record of geologic units and landforms of this enigmatic satellite remains incomplete. In this paper, we (1) present characteristics of landforms and geologic units, (2) relative and absolute ages of these units, (3) discuss open issues, and (4) suggest requirements for camera data in a future mission to Jupiter and to its satellites.

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