The sand sheet and dunes in this image, taken by NASA's 2001 Mars Odyssey spacecraft, are located on the floor of Juventae Chasma.

The sand sheet and dunes in this image, taken by NASA's 2001 Mars Odyssey spacecraft, are located on the floor of Juventae Chasma.
SuperStock offers millions of photos, videos, and stock assets to creatives around the world. This image of The sand sheet and dunes in this image, taken by NASA's 2001 Mars Odyssey spacecraft, are located on the floor of Juventae Chasma. by Piemags/PL Photography Limited is available for licensing today.

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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
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Today's VIS image shows a portion of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. Shalbatana Vallis is over 1300 km long (808 miles). This channel, and all others in this region, drain into Chryse Planitia. Orbit Number 88162 Latitude 8.96896 Longitude 318.805 Instrument VIS Captured 2021-10-29 13 34
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Today's VIS image shows a portion of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. Shalbatana Vallis is over 1300 km long (808 miles). This channel, and all others in this region, drain into Chryse Planitia. Orbit Number 89622 Latitude 8.24518 Longitude 317.972 Instrument VIS Captured 2022-02-26 18 47
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The channel-like features at the bottom of this image captured by NASA's 2001 Mars Odyssey spacecraft are part of Galaxias Fossae.
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Daedalia Planum. Today's VIS image shows a small portion of the immense lava flows that originated from Arsia Mons. Arsia Mons is the southernmost of the three large aligned volcanoes in the Tharsis region. Arsia Mons' last eruption was 10s of million years ago. The different surface textures are created by differences in the lava viscosity and cooling rates. The lobate margins of each flow can be traced back to the start of each flow or to the point where they are covered by younger flows. Flows in Daedalia Planum can be as long as 180 km (111 miles). For comparison the longest Hawaiian lava flow is only 51 km (˜31 miles) long. The total area of Daedalia Planum is 2.9 million square km - more than four times the size of Texas. Orbit Number 92102 Latitude -21.4397 Longitude 243.244 Instrument VIS Captured 2022-09-18 22 46 https //photojournal.jpl.nasa.gov/catalog/PIA25745
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Icaria Fossae. The linear features in this VIS image are tectonic graben called Icaria Fossae and are located in Terra Sirenum. 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 Icaria Fossae graben are 2115km (1314 miles) long. Orbit Number 93200 Latitude -41.7764 Longitude 243.379 Instrument VIS Captured 2022-12-18 08 42 https //photojournal.jpl.nasa.gov/catalog/PIA25847
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Pavonis Mons. This VIS image shows a cross section of the upper elevations of Pavonis Mons, including part of the summit caldera (circular region near the center of the image). Pavonis Mons is the central volcano of the three large Tharsis volcanoes. In order from north to south the volcanoes are Ascreaus Mons, Pavonis Mons and Arsia Mons. All three volcanoes form a line located along a tectonic bulge caused by extensional forces in the region. Along this trend there are increased tectonic features and additional lava flows that arose from the flanks of the volcanoes rather than just the summit. Like the other large volcanoes in the region, Pavonis Mons is a shield volcano. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. In shield volcanoes summit calderas are typically formed where the surface collapses into the void formed by an emptied magma chamber. Pavonis Mons is the smallest of the three volcanoes with a summit
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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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Lycus Sulci. Lycus Sulci is a low lying area of ridges and valleys found to the northwest of Olympus Mons. It is not yet understood how this feature formed or how it relates to the formation of Olympus Mons itself. This VIS image shows the ridge forms that are typical of this region. Orbit Number 93943 Latitude 32.5789 Longitude 215.766 Instrument VIS Captured 2023-02-17 13 53 https //photojournal.jpl.nasa.gov/catalog/PIA25932
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Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and is divided into two regions - eastern and western Candor. Candor Chasma is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits, dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides). Orbit Number 95151 Latitude -7.05226 Longitude 291.676 Instrument VIS Captured 2023-05-28 00 49
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This field of dunes is located on the floor of Brashear Crater
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. Hebes and Ophir Chasmata. Today's VIS image shows part of two chasmatas - Hebes Chasma at the top of the image and Ophir Chasma at the bottom. Both chasmata have large landslide deposits. Ophir Chasma has a large layered deposit, which has subsequently been eroded by wind and fluvial processes (bottom of image). Hebes Chasma is an inclosed basin not connected to Valles Marineris. It is 319 km long (east/west, 198 miles), 130 km wide (north/south, 81miles) and up to 8km (5 miles) deep. Ophir Chasma is approximately 317km long (197 miles) and is part of the Valles Marineris system of canyons. Orbit Number 94365 Latitude -2.67943 Longitude 286.449 Instrument VIS Captured 2023-03-24 07 37
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Today's VIS image shows a section of Mamers Valles. The channel enters a crater in the center of the image and exits at the top of the image. The channel is nearly 1000 km long (600 miles). Mamers Valles originates near Cerulli Crater in northern Arabia Terra, and after a short section near the crater where flow is to the south, flows northward to empty in Deuteronilus Mensae. The steep walls of Mamers Valles can reach heights of 1200 m (4000 feet). Orbit Number 89520 Latitude 33.5229 Longitude 17.1272 Instrument VIS Captured 2022-02-18 09 21
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Large Lava Fan on the Northwestern Flank of Olympus Mons
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This 2001 Mars Odyssey image of Capri Chasma shows multiple landslide deposits.
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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
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This VIS image shows a cross section of Pavonis Mons. Pavonis Mons is the central volcano of the three large Tharsis volcanoes. In order from north to south the volcanoes are Ascreaus Mons, Pavonis Mons and Arsia Mons. All three volcanoes form a line located along a tectonic bulge caused by extensional forces in the region. Along this trend there are increased tectonic features and additional lava flows that arose from the flanks of the volcanoes rather than just the summit. Like the other large volcanoes in the region, Pavonis Mons is a shield volcano. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. In shield volcanoes summit calderas are typically formed where the surface collapses into the void formed by an emptied magma chamber. Pavonis Mons is the smallest of the three volcanoes with a summit of only 14km (8.7 miles) and a width of 375 km (233 miles). Like most shield volcanoes the surface has a low profile. In t
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This VIS image shows the dune field on the floor of Halley Crater. Rather than small individual sand dunes, the sand here is collected into a sand sheet and dune forms have been created on that surface. Halley Crater is located on the western margin of Argyre Planitia. Orbit Number 84413 Latitude -48.8513 Longitude 300.904 Instrument VIS Captured 2020-12-24 20 22
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This VIS image crosses an unnamed crater in Terra Sabaea. The entire crater floor is covered by materials of unknown origin. Those materials are be eroded and appear to be forming chaos. The channel feature may be related to fluid activity, where the underlying material is losing water and the surface is collapsing - rather than the flow of a river over the surface. Orbit Number 88009 Latitude 2.76492 Longitude 53.6692 Instrument VIS Captured 2021-10-16 23 10
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. 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
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At the top of today's VIS image is the delta deposit on the floor of Eberswalde Crater. Deltas are formed when sediment laden rivers slow down either due to a flattening of topography, or entering a standing body of water. The reduction in velocity causes the sediments to be deposited. The main channel often diverges into numerous smaller channel that spread apart to form the typical fan shape of a delta. The Eberswalde Crater delta is one of the best preserved on Mars. Orbit Number 84562 Latitude -23.9124 Longitude 326.56 Instrument VIS Captured 2021-01-06 02 41
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Image Number: 6145-44806092Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Martian Geological FeaturesContributor:PiemagsModel Release:NoProperty Release:NoResolution:655×1373
2001 Mars Odyssey
Mars|