This 3D image shows the topography of Vesta's three craters, informally named the Snowman, obtained by the framing camera instrument aboard NASA's Dawn spacecraft on August 6, 2011. You need 3D glasses to view this image.

This 3D image shows the topography of Vesta's three craters, informally named the Snowman, obtained by the framing camera instrument aboard NASA's Dawn spacecraft on August 6, 2011. You need 3D glasses to view this image.
SuperStock offers millions of photos, videos, and stock assets to creatives around the world. This image of This 3D image shows the topography of Vesta's three craters, informally named the Snowman, obtained by the framing camera instrument aboard NASA's Dawn spacecraft on August 6, 2011. You need 3D glasses to view this image. by Piemags/PL Photography Limited is available for licensing today.

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The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Candor Chasma. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and has is divided into two regions - eastern and western Candor. Candor 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 (seen in this image), 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 71132 Latitude -6.71232 Longit
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This observation from NASA's Mars Reconnaissance Orbiter shows part of the floor of a large impact crater in the southern highlands, north of the giant Hellas impact basin.
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The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Candor Labes.
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Meridiani
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This observation from NASA's Mars Reconnaissance Orbiter (MRO) shows part of the floor of a large impact crater in the southern highlands, north of the giant Hellas impact basin.
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The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of Iani Chaos.
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The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Gale Crater.
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. Firsoff Crater - False Color. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of the floor of Firsoff Crater. Located in southern Arabia Terra, Firsoff Crater, and the neighboring Crommelin Crater, have large layered deposits on the crater floor. The circular feature at the bottom of the image is a smaller crater within Firsoff Crater. The layering of the interior deposit can be seen in the northern side of this smaller crater. Wind action has modified the large deposit. In this color combination dark blue typically indicates basaltic sand. Firsoff Crater is 90 km (56 miles) in diameter. The THEMIS VIS camera is capable of capturing color images of the Martian surface using five different color filters. In this mode of operation, the spatial reso
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This image shows part of the Nili Fossae region
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This image from NASA's Mars Reconnaissance Orbiter shows Gorgonum Basin, one of several large basins within the Terra Sirenum region of Mars. Each basin has light-toned mounds, many of which contain clays. Scientists think that Terra Sirenum once had a large lake during an epoch called the Late Noachian/Early Hesperian, and each basin filled with sediments. The water within the lake may have altered these sediments to form the clays we now observe from orbit. Ma'adim Vallis, which drains into Gusev Crater where the Spirit rover landed, drained the water from this ancient lake. Why the basin floors exhibit mounds similar to chaos regions on Mars is unknown, but could be the result of collapse and subsequent erosion within the basins.
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The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows a section of Tempe Fossae located in Tempe Terra.
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The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This false color image from NASA's 2001 Mars Odyssey spacecraft shows part of an unnamed crater in Terra Cimmeria.
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The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Iani Chaos.
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This colorful image, acquired on May 21, 2018 by NASA's Mars Reconnaissance Orbiter, shows clays within the Eridania basin region. Many scientists using orbital data have proposed that a large lake may have once existed here during the Late Noachian through Early Hesperian time periods, and then much of the water drained out to the north via Ma'adim Vallis. Understanding where and what kind of clay exists within this region using CRISM data can help scientists learn more about how long the postulated lake existed and the water chemistry within the lake. More information is available at
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This image covers a 26-kilometer-wide impact crater northeast of the Hellas impact basin as observed by NASA's Mars Reconnaissance Orbiter.
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This false color image shows a tributary channel that empties into the main Ares Vallis channel. This tributary channel is located east of Ares Vallis. Located in Margaritifer Terra, Ares Vallis is part of a large system of channels that arise from Vallis Marineris and empty into Chryse Planitia. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 63809 Latitude 4.17241 Longitude 343.459 Instrument VIS Captured 2016-05-02 20 09
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This image shows (part of) a 6-kilometer crater located on the northern slope of Bond Crater. Pole-facing gullies have eroded the northern slope of this small crater, located just west of where Uzboi Valles emanates from Bond and continues in a northerly direction. However, Hale Crater to the south has numerous gullies on its slopes and even on its central peak region. Researchers have analyzed both Bond and Hale Craters to try to determine why Bond has no gullies on its slopes, except for a small 7-km crater on the floor in its central area. (Reiss et al., 2009, PSS). The gullies in this observation have eroded into bedrock layers forming tributaries in the upper slope region and distributary channels further downslope on the debris fans. Research attributes these features to fluvial processes. (Gulick et al., 2018, Geol. Soc. London.)
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Continuing Through Iani Chaos
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This false color image shows part of Juventae Chasma. Located north of Valles Marineris, Juventae Chasma stretches for 180 kilometers (110 miles) east-west and 250 km (155 mi) north-south. Most of its floor lies 5,000 meters (16,000 feet) or more below the surrounding surface. Juventae Chasma is the source region for the outflow channel Maja Valles. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 65981 Latitude -2.2663 Longitude 298.189 Instrument VIS Captured 2016-10-28 18 05
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This false color image shows part of Mangala Fossa - the linear depression in the bottom half of the image. The bright blue tones in this image are thought to be surface frost. It is winter time and early in the morning when this image was taken. The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Orbit Number 63514 Latitude -15.1457 Longitude 219.23 Instrument VIS Captured 2016-04-08 12 54
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In this Context Camera image in Terra Cimmeria, we see a 30-kilometer diameter crater, filled-in with materials that created bedrock, and through subsequent erosion, wind-driven particles. There is a ring of exposed light-toned bedrock at the base of the crater wall. This distinctive ring suggests high winds climbing up the crater wall slope may be responsible for the erosion and the extent of bedrock exposure we see. A close-up on the southeastern part of these deposits shows a mound of bedrock with beautiful color contrasts. The variation in color represents diverse minerals in the rock. There is also a small degraded crater (about 300-meter diameter) to the left of the exposed bedrock. Fine-grained materials trapped inside the crater appear as wind-driven ripples or small dune-forms. More information is available at
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Image Number: 6145-44878396Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Mars Geological ImagingContributor:PiemagsModel Release:NoProperty Release:NoResolution:1222×1350
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