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Noctis Labyrinthus is located in the heart of Tharsis at the western end of the Valles Marineris, manifesting as a network of graben that extends in a spider-like network before coalescing into a coherent, relatively shallow graben swarm that curves in a semicircular fashion towards the south into the Claritas Rise.
Noctis Labyrinthus, on the western edge of the Valles Marineris Rift System, north of the Syria Planum and east of Pavonis Mons, is a jumbled terrain composed of huge blocks which are heavily fractured. It also contains canyons that run in different directions surrounding large blocks of older terrain.
The northwest contains Pavonis Mons and Arsia Mons, the east contains Syria Planum, the northeast includes Noctis Labyrinthus and the south-central part includes Claritas Fossae. The Phoenicis Lacus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program.
Mons (plural montes) is the Latin word for mountain; it is a descriptor term used in astrogeology for mountainous features in the Solar System. The three Tharsis Montes volcanoes are enormous by terrestrial standards, ranging in diameter from 375 km (233 mi) (Pavonis Mons) to 475 km (295 mi) (Arsia Mons). [1]
Tharsis (/ ˈ θ ɑːr s ɪ s /) is a vast volcanic plateau centered near the equator in the western hemisphere of Mars. [note 1] The region is home to the largest volcanoes in the Solar System, including the three enormous shield volcanoes Arsia Mons, Pavonis Mons, and Ascraeus Mons, which are collectively known as the Tharsis Montes.
Tharsis is a land of great volcanoes. Olympus Mons is the tallest known volcano in the Solar System; it is 100 times larger than any volcano on Earth. Ascraeus Mons and Pavonis Mons are at least 200 miles across and are over six miles above the plateau that they sit on—and, the plateau is three to four miles above the zero altitude of Mars. [4]
They are east of Noctis Labyrinthus. They display many layers in their sidewalls. Many other places on Mars also show rocks arranged in layers. Rock layers can be formed by volcanoes, wind, or water. [1] A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars. [2]
Elysium Mons is approximately 1.5 times as steep as any other Martian volcano at approximately 7-7.5°. [16] [17] The caldera at the summit of Elysium Mons is approximately 13.5 km in diameter. [16] [18] Extending past the rim of this central caldera are at least 18 sinuous channels thought to be the remnants of collapsed lava tubes and lava ...