This image from NASA's Mars Odyssey spacecraft shows some of the dunes that are located near the north polar cap. This region of dunes is part of Siton Undae.

This image from NASA's Mars Odyssey spacecraft shows some of the dunes that are located near the north polar cap. This region of dunes is part of Siton Undae.
SuperStock offers millions of photos, videos, and stock assets to creatives around the world. This image of This image from NASA's Mars Odyssey spacecraft shows some of the dunes that are located near the north polar cap. This region of dunes is part of Siton Undae. by Piemags/PL Photography Limited is available for licensing today.

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Ius Chasma. Today's VIS image shows a complete cross section of Ius Chasma. Ius Chasma is at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, wider than the United States. 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 standing water played a part in the chasma formation. The rugged floor of Ius Chasma in this image is the result of many large landslides. Orbit Number 92413
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The wind eroded surface in this image from NASA's 2001 Mars Odyssey spacecraft is located in Zephyria Planum.
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. Arabia Terra Channel. Today's VIS image shows part of a large unnamed channel located in northern Arabia Terra. Channels in this region of Arabia Terra typically flow northward into the lower elevations of Acidalia Planitia, however this channel flows east/west over the majority of its length. Orbit Number 94224 Latitude 36.8608 Longitude 28.5773 Instrument VIS Captured 2023-03-12 17 12
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Tempe Fossae. Today's VIS image is shows a portion of Tempe Fossae. The fossae are graben comprised of paired, parallel fractures with a down-dropped block of material between the fracture set. This morphology is created by extensional tectonic stresses. 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. Numerous sets of graben are visible in this THEMIS image, trending from north-northeast to south-southwest. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the north-northwest/south-southeast direction. This fossae system is located in Tempe Terra, a complexly fractured region bet
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Today's VIS image shows an unnamed channel in Terra Cimmeria. Orbit Number 87308 Latitude 2.36838 Longitude 116.9 Instrument VIS Captured 2021-08-20 05 54
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This VIS image shows a cross section of Pavonis Mons, including part of the summit caldera (circular region in the middle 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 of only 14km (8.7 miles) and a width of
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Wind is one of the remaining active processes altering the surface of Mars. In regions of long term unidirectional winds, the dust and sand is winnowed away. In places with poorly cemented surface materials the wind and entrained sand with blast the surface causing linear erosion like that seen in today's VIS image. This image is located at the equator near Gordii Dorsum. Orbit Number 77484 Latitude 5.04807 Longitude 213.038 Instrument VIS Captured 2019-06-03 08 10
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Tyrrhena Patera
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Dark Dunes in Herschel Crater
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This VIS image shows part of Cerunius Fossae. The linear depressions are fault bounded features called graben. These features form from tectonic forces that are pulling apart the surface, created space for material to slide down along the fault. Orbit Number 77308 Latitude 26.9347 Longitude 248.025 Instrument VIS Captured 2019-05-19 20 27
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This image from NASA's 2001 Mars Odyssey spacecraf shows part of the southern flank of Ascraeus Mons. Large collapse features are common in this area.
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Claritas Fossae is the dissected and fractured highland between the volcanic plains of Daedalia and Solis Planums. This image is from NASA's 2001 Mars Odyssey spacecraft.
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The extensive channel system seen is this VIS image include parts of both Sabis Vallis and Minio Vallis. The valles are just two of many channels that flow northward thru Terra Sirenum to empty into Amazonis Planitia. Sabis Vallis is 206km long (128 miles) and Minio Vallis is 88km long (55 miles). Both channels are located west of the much larger Mangala Valles. Orbit Number 81914 Latitude -5.1073 Longitude 207.895 Instrument VIS Captured 2020-06-02 02 44
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of the lava flows that make up Daedalia Planum.
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Kaiser Crater Dunes (VIS)
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Today's VIS image shows part of the floor of Orson Welles Crater. This region of the crater contains chaos. Chaos is formed where tectonic forces break the surface into blocks. Erosion along the breaks widen and deepen the valleys between creating mesas. There is evidence that this crater may once have held a lake. Orson Welles Crater is 116 km in diameter (72 miles). Orbit Number 94963 Latitude -0.688448 Longitude 314.526 Instrument VIS Captured 2023-05-12 13 20
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Juventae Chasma is an enormous box canyon which opens to the north and forms the outflow channel Maja Vallis. This image from NASA's Mars Odyssey spacecraft captures a portion of the western floor of Juventae Chasma and shows a wide variety of landforms.
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Lycus Sulci. Today's VIS image shows a portion of 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. Orbit Number 93612 Latitude 32.6141 Longitude 219.235 Instrument VIS Captured 2023-01-21 08 26 https //photojournal.jpl.nasa.gov/catalog/PIA25855
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Tractus Catena. This VIS image shows part of Tractus Catena, just one of many north/south trending tectonic graben located south and east of Alba Mons. The graben with circular pits are part of Tractus Catena. The graben without pits are part of Tractus Fossae. The pits most likely formed as a result of roof collapse into an underlying open space such as a lava tube. Orbit Number 93979 Latitude 28.6599 Longitude 257.766 Instrument VIS Captured 2023-02-20 13 00 https //photojournal.jpl.nasa.gov/catalog/PIA25940
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Kaiser Crater Dunes. This VIS image is located in Kaiser Crater and shows many individual dunes. The crater floor is visible between some of the dunes, indicating that there is a limited sand supply creating the dunes. Local winds continue to move the sand dunes across the crater floor. There are two sides to a dune, the low angle slope of the windward face and the high angle slope of the leeward side. The steep side is called the slip face. Wind blows sand grains up the low angle slope of the dunes which then fall down the slip face. In this way the whole dune moves towards the slip face. The winds blow from the windward to the leeward side of the dunes. In this image the slip faces are on the left side of the dune, so the dunes are slowly moving to the left side of this image. Kaiser Crater is located in Noachis Terra. Orbit Number 91442 Latitude -46.9786 Longitude 19.5191 Instrument VIS Captured 2022-07-26 15 07
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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 south 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 79159 Latitude 19.0493 Longitude 124.534 Instrument VIS Captured 2019-10-19 06 34
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Image Number: 6145-45058127Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Mars Geological FeaturesContributor:PiemagsModel Release:NoProperty Release:NoResolution:2476×3416
2001 Mars Odyssey
Mars|