Venus Is Far From Dead, Scientists Find

Venus looks like a planet frozen in time—hot, dry, and long assumed to be geologically dormant. Yet new modeling work now challenges that view by showing how certain rift valleys could have formed—or at least reshaped—more recently than previously thought. The findings point to tectonic processes that remain active in Venus’s interior.

Rift valleys are key tectonic markers. On Earth, they accompany plate boundary stretching and can evolve into systems such as the African Rift Valley. On Venus, comparable rift structures can stretch for thousands of kilometers, reaching up to about 10,000 km, implying the planet has experienced large-scale crustal deformation.

A major uncertainty has been timing: geoscientists have often treated many rift-related features as ancient remnants. The new study suggests a different possibility for at least some regions, where deformation may still be ongoing or have only recently slowed. This would align the surface record more closely with an active mantle.

The research team, led at ETH Zurich by Professor Taras Gerya, used a newly developed high-resolution, three-dimensional computer model to simulate rifting. Unlike earlier approaches that relied on simplified assumptions and mostly two-dimensional setups, the new framework reproduces rift geometry in greater physical detail.

In the simulations, “rift flanks”—the raised areas flanking rift valleys—form particularly when the rift system is young and either actively extending or has only just stopped. The model also indicates that rifts can widen faster than earlier estimates, at roughly 3 to 10 centimeters per year.

After movement ceases, the flanks rapidly flatten through crustal relaxation rather than the erosion-driven smoothing familiar on Earth. This helps explain how Venus can preserve steep, high-relief tectonic topography without the long-term weathering that dominates terrestrial landscapes.

The researchers further note that the simulated flank morphology matches observations from radar imaging of Venus’s surface collected by NASA’s Magellan mission in the 1990s. Such consistency strengthens the argument that Venus’s rifting is not merely ancient history.

Overall, the study concludes that Venus remains geologically active and that its interior is more dynamic than previously believed. The results can help prioritize targets for future exploration aimed at mapping where tectonics may still be reshaping the surface.

With NASA and ESA planning new Venus missions, these insights arrive at a crucial moment. Understanding active rifting will also inform broader questions about how rocky planets evolve—information relevant even to the search for rocky exoplanets.

Keywords

Venus, rift valleys, tectonic activity, 3D geodynamic modeling, rift flanks, crustal relaxation, Magellan radar, planetary geology, Nature Geoscience, EnVision