This image from NASA's 2001 Mars Odyssey spacecraft shows two small tributaries, just east of where they join Shalbatana Vallis.

This image from NASA's 2001 Mars Odyssey spacecraft shows two small tributaries, just east of where they join Shalbatana Vallis.
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The top of the Cerulli Crater rim is located in the center of the VIS image. The top half of the image is the interior rim, with numerous channels dissecting it and flowing down onto the crater floor. The lower half of the image is the outer crater rim. Orbit Number 78314 Latitude 31.1413 Longitude 22.0425 Instrument VIS Captured 2019-08-10 16 41
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Channels are a common feature on the margin of Terra Cimmeria where the elevation changes from highland to northern lowlands in this image captured by NASA's Mars Odyssey.
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In regions of poorly cemented surface materials it is possible to create large features due to just the action of the wind. The equatorial region between Olympus Mons and Apollinaris Mons is dominated by wind etched regions. This region east of Apollinaris Mons contains just such a terrain. The direction of the wind aligns with the ridges and valleys. The dominant wind direction in this region is southeast to northwest; however, other wind directions can occur within a localized region.The top of this VIS image follows the regional trend, with a smaller central surface indicating winds perpendicular to the prevailing direction. Orbit Number 72333 Latitude -10.2083 Longitude 179.736 Instrument VIS Captured 2018-04-05 02 02
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This unnamed crater near Timoshenko Crater has been breached by a channel
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Windstreak
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Moving eastward from the previous image, we continue to see the northern floor and rim of Gale Crater and the northern part of Mt. Sharp. This image from NASA's Mars Odyssey spacecraft shows a weathered region of the lower elevations of Mt. Sharp.
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Marikh Vallis is the name given to the channels seen in this image of Noachis Terra as seen by NASA's 2001 Mars Odyssey spacecraft.
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Rim Channels
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows several linear depressions that cross an unnamed crater. The depressions are tectonic fractures that are hundreds of km long.
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This VIS image shows a small section of Indus Vallis. Indus Vallis is located in northern Terra Sabaea. Orbit Number 77727 Latitude 18.7218 Longitude 40.0134 Instrument VIS Captured 2019-06-23 08 30
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Small channels dissect this region near Nectaris Fossae
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Today's VIS image shows some of the linear depressions that comprise Nili Fossae. Nili Fossae is the name of a collection of curved faults and down-dropped blocks of crust between the faults. The fossae, or 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 88158 Latitude 20.507 Longitude 72.6076 Instrument VIS Captured 2021-10-29 05 43
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Slope Streaks
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This small unnamed channel is located in southern Tyrrhena Terra as seen by NASA's 2001 Mars Odyssey spacecraft.
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The channels in this image captured by NASA's 2001 Mars Odyssey spacecraft are dissecting a slope near Huygens Crater.
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This image from NASA's 2001 Mars Odyssey spacecraft shows the region just northwest of yesterday's image of Gale Crater. This region is dissected by small channels.
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The dunes in this image are located on the floor of an unnamed crater in Tyrrhena Terra as seen by NASA's 2001 Mars Odyssey spacecraft.
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This image shows part of the southern flank of Pavonis Mons. Several faults run from the left to the right side of the image. Lava flows, and the lava collapse features at the bottom of the image are aligned with the down hill direction (in this case from the top of the image to the bottom). Near the top of the image there are collapse features that run along the faults. The fault may have been been a location for lava tube development. Pavonis Mons is one of the three aligned Tharsis Volcanoes. The four Tharsis volcanoes are Ascreaus Mons, Pavonis Mons, Arsia Mons, and Olympus Mars. All four are shield type volcanoes. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. The Hawaiian islands on Earth are shield volcanoes. The three aligned volcanoes are located along a topographic rise in the Tharsis region. Along this trend there are increased tectonic features and additional lava flows. Pavonis Mons is the smallest of th
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Image Number: 6145-58967617Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Martian Crater TopographyContributor:PiemagsModel Release:NoProperty Release:NoResolution:729×1556
2001 Mars Odyssey
Mars|