Geology of Venus

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The geology of Venus is the scientific study of the planet's surface, crust, and interior. Approximately 75% of the surface is composed of bare rock, predominantly volcanic bedrock, with some areas featuring thin and patchy layers of regolith.

Volcanism appears to be the dominant agent of geological change on Venus. The planet's surface is characterized by large regions of highly deformed terrain, known as tesserae, which are folded and fractured in two or three dimensions. Arachnoids, features resembling a spider's web, also dominate the landscape.

Despite its relatively flat topography, with only 1 meter (±2 feet) of elevation above the median radius of 6,052 kilometers (3,761 miles), Venus has several notable mountain ranges surrounding Lakshmi Planum. Maxwell Montes, Akna Montes, and Freya Montes are among the most prominent elevations, reaching heights of up to 11 kilometers (6.8 miles). The inclination of these mountains is relatively low, with a maximum angle of 30 degrees recorded in Danu Montes and Themis Regio.

Highlands cover approximately 10% of Venus' surface, defined as areas greater than 2 kilometers (1.2 miles) in elevation. These regions are characterized by high concentrations of pyrite, an iron sulfide mineral. The Highlands also exhibit unique radar signatures, making them particularly effective at reflecting signals and appearing bright on images.

In contrast to the Highlands, the plains cover most of Venus' surface, with only 30% extending beyond 10 kilometers in height. This is significantly lower than Earth's oceanic crust, which separates the terrestrial mountains from the highest peaks. The low elevation of these regions suggests that they would experience relatively stable temperatures, whereas areas above 2 kilometers in elevation are subject to significant temperature fluctuations.

The surface composition of Venus is primarily composed of solidified lava flows, with estimates suggesting that around 85% of the planet's surface is made up of such material. However, this does not necessarily indicate ongoing volcanic activity, as the last major period of widespread volcanism occurred approximately 800 million years ago. The presence of impact craters, although relatively few in number compared to Earth, provides evidence for a geologically active past.

The Venusian atmosphere plays a crucial role in shaping its surface features. The dense atmosphere prevents smaller meteorites from reaching the surface, causing them to disintegrate