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The surface of Venus hosts hundreds of circular to elongate features, ranging from 60 to 2600 km, and averaging somewhat over 200 km, in diameter. These enigmatic structures have been termed “coronae” and attributed to either tectonovolcanic or impact-related mechanisms. A quantitative analysis of symmetry and topography is applied to coronae and similarly sized craters to evaluate the hypothesized impact origin of these features. Based on the morphology and global distribution of coronae, as well as crater density within and near coronae, we reject the impact origin for most coronae. The high level of modification of craters within coronae supports...

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