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Venus: Interpreting the spatial distribution of volcanically modified craters
Author(s) -
O'Rourke Joseph G.,
Wolf Aaron S.,
Ehlmann Bethany L.
Publication year - 2014
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1002/2014gl062121
Subject(s) - impact crater , geology , venus , volcano , lava , volcanism , magmatism , shield volcano , lunar craters , volcanology , spatial distribution , geophysics , astrobiology , petrology , earth science , geomorphology , seismology , remote sensing , tectonics , physics
To understand the impact cratering record on Venus, we investigate two distinct resurfacing styles: localized, thin flows and large shield volcanoes. We statistically analyze the size‐frequency distribution of volcanically modified craters and, using Monte Carlo simulations, their spatial distribution. Lava flows partially fill most craters, darkening their floors in radar images. We find that a model featuring localized, thin flows occurring throughout geologic time predicts their observed distribution. Individual flows may be morphologically indistinguishable, but, combined, they cover large provinces. Recent mantle plumes may drive a small amount of hot spot magmatism that produces the observed clusters of large shield volcanoes and obviously embayed craters. Ultimately, our analysis demonstrates that two styles of volcanism are needed to explain the observed properties of impact craters and that catastrophic resurfacing is not required.