Mars Geological Features

Images of Martian landscapes captured by spacecraft, showcasing geological formations such as valleys, ridges, and lava flows on the surface of Mars.

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$The linear depressions in this VIS image are part of the Cerberus Fossae fracture system. The system is made up of parallel graben created by tectonic forces pulling the crust apart. The entire system is 1235km long (767 miles). Orbit Number 79270 Latitude 8.68461 Longitude 163.521 Instrument VIS Captured 2019-10-28 09 53$

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This ridge of material on the northern end of Gordii Dorsum is being reduced in size by the erosive effect of the wind in this image captured by NASA's Mars Odyssey.

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$This NASA Mars Odyssey image covers a tract of plateau territory called Ophir Planum. The most obvious features in this scene are the fractures (ranging from 1 to 5 km wide) running from the upper left to lower right.$

$These fractures and graben are part of Sirenum Fossae as seen by NASA's 2001 Mars Odyssey spacecraft.$

$Lava channels and tectonic fractures are both found in the Tharsis region as shown in this image from NASA's Mars Odyssey.$

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This image captured by NASA's 2001 Mars Odyssey spacecraft shows more of the extensive lava flows in Daedalia Planum.

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The complex region of channels at the top of this image, captured by NASA's 2001 Mars Odyssey spacecraft, are lava channels. These channels are called Olympica Fossae.

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$Tractus Catena is a series of collapse pits and fractures south of Alba Mons as seen in this image from NASA's 2001 Mars Odyssey spacecraft. The collapse pits, which run in two directions in this image, are typically indicative of volcanic lava tubes.$

$Ceraunius Fossae is the region of fractures and volcanic flows south of Alba Mons shown in this image captured by NASA's Mars Odyssey.$

$The fractures in this image are part of the large fracture system that surrounds Alba Mons as seen by NASA's 2001 Mars Odyssey spacecraft.$

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$Tithonium and Ius Chasmata. Ius and Tithonium Chasmata are located at the western end of Valles Marineris. Tithonium Chasma is north of Ius Chasma. Valles Marineris is over 4000 kilometers long (2495 miles), almost as wide as the United States. Ius Chasma is almost 840 kilometers long (522 miles), 120 kilometers wide and over 8 kilometers deep. Tithonium Chasma is 803 km (499 miles) long. In comparison, the Grand Canyon in Arizona is about 175 kilometers long (109 miles), 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. Landslides have enlarged the canyon walls and created deposits on the canyon floor. Weathering of the surface and influx of dust and sand have modified the canyon floor, both creating and modifying layered materials. There are many features that indicate flowing and standing water played a part in the chasma formation. The rugg$

$Just as on Earth, volcanism and tectonism are found together on Mars. In this image from NASA's 2001 Mars Odyssey spacecraft the ridges and fractures of Claritas Fossae are affecting or perhaps hosting the volcanic flows of Solis Planum.$