Central pit and dome craters - Exposing the interiors of Ganymede and Callisto

Details Central pit and dome craters - Exposing the interiors of Ganymede and Callisto Central pit and dome craters - Exposing the interiors of Ganymede and Callisto

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....98.7475s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. E4, p. 7475-7498.

Physics

43

Callisto, Ganymede, Planetary Craters, Satellite Surfaces, Domes (Geology), Geomorphology, Pits (Excavations), Planetary Crusts, Jupiter, Satellites, Ganymede, Callisto, Craters, Domes, Interior, Icy Bodies, Depth, Morphology, Size, Comparisons, Impact Effects, Rims, Description, Structure, Crust, Ice, Rheology, Uranus, Titania, Models, Ursula, Diameter, Width, Topography, Ashima, Central Pits, Formation, Osiris, Enkidu, Origin, Uplift, Moon

Scientific paper

Central pit craters on Ganymede and Callisto are an unusual crater class, perhaps related to the unusual properties of water ice. The domes and pits form rapidly, on the time scale of the impact itself, rather than by long-term, post-impact intrusion or extrusion. The bright domes in pit craters are most simply explained as the uplift and exposure of relatively ice-rich material from depths of approximately 3.5 to 5 km during impact. The unusual pit morphology on icy satellites may be the result of impact into crust that is mechanically much weaker at shallow depth than on rocky bodies such as the moon. Because crater morphology is strongly dependent on ice-rock composition, the similarity of pit and dome dimensions on Ganymede and Callisto indicates that the structure and rheology of the crusts of these bodies are very similar, and have been for several billion years. Pit crater morphology indicates that the crusts of both satellites are probably ice-rich and differentiated.

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