Bizarre surface formations on Venus, termed coronae, are shedding light on the planet’s enigmatic interior. Utilizing data from the NASA Magellan spacecraft, which operated until 1994, a team led by Anna Gulcher from the University of Freiburg has developed advanced 3D models of these structures to enhance our understanding of Venus’ geodynamics.
Exploring the Coronae
The research team analyzed data from the Magellan spacecraft’s radar sensors to examine the coronae’s surrounding topography and gravitational signatures. Their findings, presented at the European Geosciences Union’s 2026 General Assembly in Vienna, reveal that the coronae exhibit a remarkable variety in size, morphology, and tectonic settings. This diversity suggests that they do not arise from a single formation mechanism but are instead indicative of a spectrum of dynamic geological processes.
Key Findings on Geodynamics
The updated database now includes 741 coronae across Venus’ surface. These formations are characterized as large circular systems of fractures, believed to be the surface manifestation of hot material plumes rising from the planet’s interior. Gulcher emphasized that understanding these structures is vital for deciphering Venus’ geodynamic regime and for assessing whether similar processes occurred on early Earth.
Insights into Tectonic Activity
By integrating gravity and topographic data with geodynamic simulations, the study identified potential warm mantle upwellings beneath 52 coronae, providing compelling evidence of varied plume-related tectonic processes. Gulcher noted that current gravity data may overlook many active tectonic signals, suggesting that Venus could be experiencing more widespread geological activity than previously recognized.
Comparative Planetology
The coronae range in diameter from 60 km to over 2000 km. The circular nature of these formations is thought to result from circular features originating from the interior, such as magma plumes that cause significant crustal uplift. This mantle convection process, which involves the movement of the mantle layer, is believed to play a crucial role in the planet’s geological evolution.
Gulcher pointed out that while Venus exhibits structures reminiscent of Earth, significant differences exist, particularly concerning the recycling of carbon and the presence of water. The absence of large water oceans on Venus likely limits its capacity for tectonic activity and carbon recycling, contrasting sharply with Earth’s dynamic plate tectonics.
Future missions, including VERITAS and EnVision, are expected to provide unprecedented insights into the surface and subsurface structures of Venus, enhancing our understanding of these intriguing formations.
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