TY - JOUR
T1 - Venus
T2 - Interpreting the spatial distribution of volcanically modified craters
AU - O'Rourke, Joseph G.
AU - Wolf, Aaron S.
AU - Ehlmann, Bethany L.
N1 - Publisher Copyright:
©2014. American Geophysical Union. All Rights Reserved.
PY - 2014/12/16
Y1 - 2014/12/16
N2 - 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.
AB - 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.
KW - Venus
UR - http://www.scopus.com/inward/record.url?scp=84921539242&partnerID=8YFLogxK
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U2 - 10.1002/2014GL062121
DO - 10.1002/2014GL062121
M3 - Article
AN - SCOPUS:84921539242
SN - 0094-8276
VL - 41
SP - 8252
EP - 8260
JO - Geophysical Research Letters
JF - Geophysical Research Letters
IS - 23
ER -