We examine the importance of localized volcanism in resurfacing on Venus by analyzing the results of geologic mapping of a 12° × 12° area at the full resolution of Magellan SAR data. Resurfacing due to corona-, ridge-, and small volcano-related volcanism accounts for 27%, 6%, and 10% respectively of the mapped area. Mapping at the resolution of Magellan data, rather than a regional scale, gives corona-related flow unit areas that can differ individually by almost an order of magnitude, with a total increase of 28%, and more than three times as many identifiable units. A total of 2919 small volcanoes or vents less than 10 km in diameter were identified in the F-Map, with a mean diameter of 1.59 (s.d. = 1.08) km and densities of up to 36 small volcanoes per 50 km². Taken together, coronae, ridge eruptions, and small volcanoes probably make a significant contribution to resurfacing on Venus.