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Morphology and Scaling of Ejecta Deposits on Icy SatellitesContinuous ejecta deposits on Ganymede consist of two major units, or facies: a thick inner hummocky pedestal facies, and a relatively thin outer radially scoured facies defined also by the inner limit of the secondary crater field. Both ejecta facies have a well-defined power-law relationship to crater diameter for craters ranging from 15 to approx. 600 km across. This relationship can be used to estimate the nominal crater diameter for impact features on icy satellites (such as palimpsests and multiring basins) for which the crater rim is no longer recognizable. Ejecta deposits have also been mapped on 4 other icy satellites. Although morphologically similar to eject deposits on the Moon, ejecta deposits for smaller craters are generally significantly broader in extent on the icy satellites, in apparent defiance of predictions of self-similarity. A greater degree of rim collapse and enlargement on the Moon may explain the observed difference.
Document ID
20030012595
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Schenk, Paul M. (Lunar and Planetary Inst. Houston, TX United States)
Ridolfi, Francis J. (Lunar and Planetary Inst. Houston, TX United States)
Bredekamp, Joe
Date Acquired
August 21, 2013
Publication Date
January 1, 2002
Publication Information
Publication: Geophysical Research Letters
Volume: 29
Issue: 12
ISSN: 0094-8276
Subject Category
Lunar and Planetary Science and Exploration
Report/Patent Number
LPI-Contrib-1113
Funding Number(s)
CONTRACT_GRANT: NASW-4574
Distribution Limits
Public
Copyright
Other