Modification of premare impact craters by volcanism and tectonism

Details Modification of premare impact craters by volcanism and tectonism Modification of premare impact craters by volcanism and tectonism

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975moon...12..449b&link_type=abstract

The Moon, vol. 12, Apr. 1975, p. 449-461.

Mathematics

Logic

3

Lunar Craters, Meteorite Craters, Tectonics, Volcanology, Astronomical Models, Geomorphology, Lunar Maria, Lunar Photographs

Scientific paper

Many 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.

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