DIX Planetary Science Seminar

The surface of Venus is primarily characterized by volcanic morphologies, such as shield volcanoes, volcanic plains, and other volcanic related structures as coronae, novae and arachnoids. Although volcanism has been the main morphogenetic agent that reshaped the surface of Venus, the evolution of this activity throughout the planet's geological history remains largely unknown. Several studies have provided hints of geologically recent volcanic activity, with two recent works reporting the first direct evidence of morphological changes on the surface of Venus during the Magellan mission in the 1990s. In particular, possible new lava flows have been observed by comparing radar images acquired by Magellan in the same area at different times. These significant changes in radar backscatter were detected in two different regions of Venus: along the western flank of Sif Mons, one of the planet's major shield volcanoes, and in Niobe Planitia, a vast volcanic plain. These findings suggest that Venus is still geologically active today, and its volcanic activity may even be comparable to that of Earth. Such implications are fundamental for understanding Venus's internal processes and its current state of activity.