We review recent developments in the study of volcanism and tectonics onVenus. Venus's crust is basaltic, dry, and probably about 30 km thick. Themantle convects, giving rise to plumes, and has a similar composition and meantemperature (∼1300°C), but a higher viscosity (∼10²⁰ Pas), than that of the Earth. Inferred melt generation rates constrain thelithospheric thickness to between 80 and 200 km. The elastic thickness of thelithosphere is about 30 km on average. The present-day lack of plate tectonicsmay be due to strong faults and the high viscosity of the mantle. Most of thedifferences between Earth and Venus processes can be explained by the absenceof water.

Venus underwent a global resurfacing event 300–600 Ma ago, the causeand nature of which remains uncertain. The present-day surface heat flux onVenus is about half the likely radiogenic heat generation rate, which suggeststhat Venus has been heating up since the resurfacing event.