Mapping the Thermal Structure and the Seismogenic Thickness of Venus

Abstract

The young surface of Venus exhibits a wide diversity of tectonic features, including rift zones that extend for thousands of kilometers [1], wrinkle ridges distributed across the planet [2], and hundreds of coronae that may be associated with regional subduction [3,4]. Additionally, there is a growing body of observations suggesting that Venus is geologically active at present [e.g., 5,6]. Consequently, it is likely that Venus is also a seismically active planet [7]. However, very little is known about its seismicity, primarily due to the lack of seismic data. In the meantime, by leveraging other geophysical constraints, we can begin to investigate some of Venus’s seismic properties. Such analyses are essential for planning future seismic-focused missions to Venus [e.g., 8].