Venus: Interpreting the spatial distribution of volcanically modified craters. Issue 23 (11th December 2014)

• Record Type: Journal Article
• Authors: O'Rourke, Joseph G.; Wolf, Aaron S.; Ehlmann, Bethany L.
• Is Part Of: Geophysical research letters. Volume 41:Issue 23(2014:Dec.)
• Page Start: 8252
• Page End: 8260
• Publication Date: 2014-12-11
• Subjects: Venus; Geophysics -- Periodicals; Planets -- Periodicals; Lunar geology -- Periodicals; 550
• DOI: 10.1002/2014GL062121
• Languages: English
• ISSNs: 0094-8276

Abstract

Abstract: 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. Key Points: Producing the modern cratering record on Venus requires two types of volcanism Thin, morphologically similar flows dominate and tall volcanoes are secondary Noncatastrophic processes can explain the distribution of modified craters