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Modification of premare impact craters by volcanism and tectonismMany lunar craters greater than 10 km in diameter exhibit a variety of morphological characteristics which are not produced by meteorite impact or meteorite erosion. Most such craters are located in or near the margins of the maria. Although some could have resulted from processes such as cauldron resurgence, caldera formation, or ring dike emplacement, most have formed by modification of impact craters by endogenic processes including erosion by flowing lava, fissure volcanism, plutonism, and uplift of crater floors along ring fractures of impact origin.
Document ID
19750057675
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Brennan, W. J.
(New York, State University Geneseo, N.Y., United States)
Date Acquired
August 8, 2013
Publication Date
April 1, 1975
Publication Information
Publication: The Moon
Volume: 12
Subject Category
Lunar And Planetary Exploration
Accession Number
75A41747
Funding Number(s)
CONTRACT_GRANT: NAS9-12770
Distribution Limits
Public
Copyright
Other

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