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How did the Tharsis rise affect the crust of Mars?
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Mars
An especially serene view of Mars (Tharsis side), a composite of images taken by the Mars Global Surveyor spacecraft in April 1999. The northern polar cap and encircling dark dune field of Vastitas Borealis are visible at the top of the globe. White water-ice clouds surround the most prominent volcanic peaks, including Olympus Mons near the western limb, Alba Patera to its northeast, and the line of Tharsis volcanoes to the southeast. East of the Tharsis rise can be seen the enormous near-equatorial gash that marks the canyon system Valles Marineris.
The Tharsis rise, a massive volcanic dome on Mars, significantly deformed the planet's crust through the immense stresses generated by its size and weight.12
This geological process resulted in two primary structural features:
- Radial Fractures: A vast system of fractures radiates outward from the center of the rise, covering approximately one-third of the planet. These fractures are believed to have formed due to the crustal stresses induced by the presence of the massive dome.2
- Compressional Ridges: The crust surrounding the rise exhibits compressional ridges, which serve as further evidence of the deformation caused by the uplift.1
Additionally, the radial faulting associated with the Tharsis rise is thought to have contributed to the development of the Valles Marineris canyon system. The rise itself is composed of a vast accumulation of volcanic rock, likely formed through a combination of tectonic uplift and the extensive buildup of lava flows.12