Recent three-dimensional computer simulations conducted by researchers at ETH Zurich suggest that Venus is a geologically active planet with a significantly more dynamic interior than previously believed. While the planet was long considered geologically frozen, findings published in the journal Nature Geoscience indicate that massive fractures on the surface may have formed recently and could still be expanding.
New Simulations Challenge Venus’s Frozen Reputation
The research team, led by Professor of Geodynamics Taras Gerya and Xi Yang, utilized high-resolution 3D modeling to analyze rift valleys on the Venusian surface. These valleys, which can span up to 10,000 kilometers, are lowland regions flanked by mountainous ridges known as rift flanks. According to the study, the physical characteristics of these flanks—specifically their height and width—serve as indicators of a rift’s geological age.
Understanding Rift Flank Dynamics
The simulations demonstrate that rift flanks remain broad and high when a rift system is geologically young and either currently moving or only recently inactive. As a system ages, these flanks become lower and narrower. Unlike Earth, where such features are primarily worn down by erosion, the researchers determined that Venusian rift flanks flatten due to crustal relaxation
after movement ceases.
These findings provide a new framework for interpreting surface imagery captured by NASA’s Magellan spacecraft. Launched in 1989, the Magellan probe imaged more than 98% of the Venusian surface during its mission in the 1990s. The team compared their 3D models to this archival data, noting that the broad, high rift flanks produced by their simulations match the features visible in the Magellan maps. This observational support suggests that the rifts are widening at a rate of 3 to 10 centimeters per year, a speed faster than previous scientific estimates had suggested.
Implications for Future Planetary Exploration
The confirmation of ongoing tectonic activity, combined with previous evidence of volcanic activity—such as changes observed in a volcanic vent at Maat Mons in 1991—challenges the long-held view of Venus as a geologically stagnant world.
These results are expected to assist space agencies in prioritizing regions for upcoming exploration. NASA and the European Space Agency (ESA) are currently preparing missions to investigate the planet, including the European EnVision mission, which is planned for the early 2030s. Professors Taras Gerya and Paul Tackley of ETH Zurich are participating in the development of instrumentation for these future missions, which aim to survey the planet from its core to the upper atmosphere.
Broader Scientific Context
Beyond the study of Venus, the researchers believe their methodology has significant implications for broader astrophysical research. By establishing a better understanding of the tectonic processes that shape terrestrial planets, the team hopes to create more effective tools for detecting and analyzing rocky exoplanets located far beyond our Solar System.
The findings mark a shift in how geoscientists perceive the evolution of our planetary neighbor. While the formation timing of these rifts was previously estimated at over 100 million years ago, leading many to view them as remnants of the distant past, the new modeling provides evidence that the planet is likely still in geologic motion.
For further details on the study’s methodology and findings, see the published research at SCI or explore additional analysis regarding the geological activity of Venus.
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