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impact cratering experiments in bingham materials and the morphology of craters on mars and ganymedeResults from a series of laboratory impacts into clay slurry targets are compared with photographs of impact craters on Mars and Ganymede. The interior and ejecta lobe morphology of rampart-type craters, as well as the progression of crater forms seen with increasing diameter on both Mars and Ganymede, are equalitatively explained by a model for impact into Bingham materials. For increasing impact energies and constant target rheology, laboratory craters exhibit a morphologic progression from bowl-shaped forms that are typical of dry planetary surfaces to craters with ejecta flow lobes and decreasing interior relief, characteristic of more volatile-rich planets. A similar sequence is seen for uniform impact energy in slurries of decreasing yield strength. The planetary progressions are explained by assuming that volatile-rich or icy planetary surfaces behave locally in the same way as Bingham materials and produce ejecta slurries with yield strenghs and viscosities comparable to terrestrial debris flows. Hypothetical impact into Mars and Ganymede are compared, and it is concluded that less ejecta would be produced on Ganymede owing to its lower gravitational acceleration, surface temperature, and density of surface materials.
Document ID
19820048255
Document Type
Conference Proceedings
Authors
Fink, J. H.
(Arizona State Univ. Tempe, AZ, United States)
Greeley, R.
(Arizona State University Tempe, AZ, United States)
Gault, D. E.
(Murphys Center for Planetology Murphys, CA, United States)
Date Acquired
August 10, 2013
Publication Date
January 1, 1982
Subject Category
LUNAR AND PLANETARY EXPLORATION
Meeting Information
Lunar and Planetary Science Conference(Houston, TX)
Funding Number(s)
CONTRACT_GRANT: NAGW-56
CONTRACT_GRANT: NAGW-132
CONTRACT_GRANT: NSG-7548
Distribution Limits
Public
Copyright
Other