Martian Geological Features

Images depicting various geological formations on Mars including faults, grabens, and lava flows, showcasing textures and structures in grayscale.

This VIS image is located in the central portion of Hephaestus Fossae. Hephaestus Fossae is a complex channel system in Utopia Planitia near Elysium Mons. It has been proposed that the channel formed by the release of melted subsurface ice during the impact event that created a large crater southeast of this image. Additionally, the nearby Elysium volcanic center created subsurface heating that may have played a part in creating both Hephaestus Fossae and Hebrus Valles to the north. Orbit Number 82079 Latitude 18.8004 Longitude 124.5724 Instrument VIS Captured 2020-06-15 16 56

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The linear depressions in today's VIS image are part of Nili Fossae. Nili Fossae is a collection of curved faults and down-dropped blocks of crust between the faults called graben. Graben are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. The Nili Fossae graben lie northeast of the large volcano Syrtis Major and northwest of the ancient impact basin Isidis Planitia. The troughs, which can be almost 500 meters (1,600 feet) deep , make concentric curves that follow the outline of Isidis Planitia. The graben likely formed as the crust sagged under the weight of lava flows filling the Isidis Planitia impact basin. Orbit Number 94784 Latitude 18.0574 Lo

$Cyane Sulci. Today's VIS image shows a portion of Cyane Sulci. Located to the northeast of Olympus Mons, Cyane Sulci is a complexly fractured region of material inundated on its margins by volcanic flows. Orbit Number 93905 Latitude 23.0568 Longitude 233.41 Instrument VIS Captured 2023-02-14 10 45 https //photojournal.jpl.nasa.gov/catalog/PIA25924$

$. Fossae. Today's VIS image shows an unnamed region of fractures and graben. Located south of Solis Planum, between Claitas Fossae and Coracis Fossae, this region of fossae has the same appearance and graben orientation of the bordering named Fossae. Fossae are long linear depressions called graben and are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Orbit Number 91764 Latitude -36.7342 Longitude 272.1 Instrument VIS Captured 2022-08-22 02 55$

$The fracture system shown in this image from NASA's Mars Odyssey is on the northern margin of the Kasei Valles lowland. Fractures like this can become chaos with continued downdropping of blocks and widening fractures.$

$This image from NASA's Mars Odyssey captures Mangala Fossa. Mangala Fossa is a graben, which in geologic terminology translates into a long parallel to semi-parallel fracture or trough.$

$Today's VIS image shows the part of the northern side of Tithonium Chasma. Tithonium Chasma is at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, almost as wide as the United States. Tithonium Chasma is almost 810 kilometers long (499 miles), 50 kilometers wide and over 6 kilometers deep. In comparison, the Grand Canyon in Arizona is about 175 kilometers long, 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. Landslides have enlarged the canyon walls and created deposits on the canyon floor. Weathering of the surface and influx of dust and sand have modified the canyon floor, both creating and modifying layered materials. The layered materials are at the bottom of the image, while a small landslide deposit can be seen in the center of the image. Orbit Number 90884 Latitude -4.28132 Longitude 271.232 Instrumen$

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Dust devil tracks criss-cross the surface in this image captured by NASA's 2001 Mars Odyssey spacecraft.

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$These stars found on the floor of Ceres' Occator Crater belong to the Vinalia Faculae. The faculae are deposits of salts, in particular sodium carbonate, possibly extruded through fractures connecting the surface to a deep reservoir of salty liquid. The images used in this montage were obtained by NASA's Dawn spacecraft in June 2018 from an altitude of about 21 miles (34 kilometers). NASA announced the conclusion of Dawn's mission operations was Oct. 31, 2018, when the spacecraft depleted its hydrazine. The center of this feature is located at about 20.2 degrees north latitude and 241.3 degrees east longitude, in the eastern part of Occator Crater. Occator Crater is named after the Roman agricultural deity of the harrowing, a helper of Ceres, the goddess of agriculture, grain crops, fertility and motherly relationships.$

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This VIS image shows part of Sisyphi Cavi located in Noachis Terra near the south polar cap. Cavi are defined as steep sided depressions. Gullies dissect the cliff tops and dunes are found on the floors of the depressions. Orbit Number 76175 Latitude -71.7607 Longitude 1.72024 Instrument VIS Captured 2019-02-15 12 27

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$Arsia Mons Flank. The three large aligned Tharsis volcanoes are Arsia Mons, Pavonis Mons and Ascreaus Mons (from south to north). There are collapse features on all three volcanoes, on the southwestern and northeastern flanks. This alignment may indicate a large fracture/vent system was responsible for the eruptions that formed all three volcanoes. This VIS image shows part of the northwestern flank of Arsia Mons, west of the aligned fracture system. The scalloped depressions and lines of craters are most likely created by collapse of the roof of lava tubes. Lava tubes originate during eruption event, when the margins of a flow harden around a still flowing lava stream. When an eruption ends these can become hollow tubes within the flow. With time, the roof of the tube may collapse into the empty space below. The tubes are linear, so the collapse of the roof creates a linear depression. In this region, the complexity of the collapse and faulting has created a unique surface. This regio$

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$Today's VIS image shows the southern cliffside of Tithonium Chasma (top of image) and the complete cross section of Ius Chasma (center of image). Ius Chasma and Thithonium Chasma are at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, wider than the United States. Tithonium Chasma is 803 kilometers long (499 miles) while Ius Chasma is almost 850 kilometers long (528 miles), 120 kilometers wide and over 8 kilometers deep. In comparison, the Grand Canyon in Arizona is about 175 kilometers long, 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. Landslides have enlarged the canyon walls and created deposits on the canyon floor. Weathering of the surface and influx of dust and sand have modified the canyon floor, both creating and modifying layered materials. There are many features that indicate flowing and standi$

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