Venusian Volcanic Xenolandscapes

Abstract

The study of Venusian xenolandscapes presents a significant scientific challenge due to their limited exploration and the specificity of available data. Research primarily focuses on impact ring structures and volcanic formations, which serve as key subjects for xenogeological and xenogeomorphological interpretations. Using radar imagery from interplanetary spacecraft, detailed relief models of Venus have been constructed, enabling the identification of numerous volcanic and tectonic features, their distribution, and characteristics. Venus exhibits prolonged volcanic activity, driven by its thermal potential. Approximately 80 % of the planet's surface is covered with extrusive volcanic materials, including lava plains – the largest in the Solar System. Notably, data from the Magellan mission revealed over 1 660 volcanic features of varying scales, ranging from small shield volcanoes to large coronae and lava channels. The primary types of volcanic plains – heavily deformed, moderately deformed, and undeformed – reflect successive stages of planetary evolution. The Venusian crust is predominantly basaltic and lacks water, which defines its unique geodynamic properties, including the absence of plate tectonics and the dominance of sub-lithospheric volcanic mechanisms. The concentration of volcanic structures in regions such as Beta, Atla, and Themis indicates ongoing activity, supported by localized thermal anomalies, radar data, and analyses of lava flows. Additionally, the stability of Venus’s global cloud layer, primarily composed of sulfuric acid droplets, further suggests persistent volcanism. Investigations into Venusian volcanic structures enhance our understanding of planetary evolution and geodynamic processes operating under high pressure and temperature conditions. Future missions and advancements in radiometric technologies promise new opportunities for monitoring contemporary volcanic activity and detailed surface mapping of Venus.