Much of Mars surface is covered by fine-grained materials that hide the bedrock, but in this scene from NASA's Mars Reconnaissance Orbiter, the bedrock is well exposed except where covered by sand dunes.

Much of Mars surface is covered by fine-grained materials that hide the bedrock, but in this scene from NASA's Mars Reconnaissance Orbiter, the bedrock is well exposed except where covered by sand dunes.
SuperStock offers millions of photos, videos, and stock assets to creatives around the world. This image of Much of Mars surface is covered by fine-grained materials that hide the bedrock, but in this scene from NASA's Mars Reconnaissance Orbiter, the bedrock is well exposed except where covered by sand dunes. by Piemags/PL Photography Limited is available for licensing today.

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The feature that appears bright blue at the center of this scene is NASA's Curiosity Mars rover on the northwestern flank of Mount Sharp, viewed by NASA's Mars Reconnaissance Orbiter. Curiosity is approximately 10 feet long and 9 feet wide (3.0 meters by 2.8 meters). The view is a cutout from observation ESP_050897_1750 taken by the High Resolution Imaging Science Experiment (HiRISE) camera on the orbiter on June 5, 2017. HiRISE has been imaging Curiosity about every three months, to monitor the surrounding features for changes such as dune migration or erosion. When the image was taken, Curiosity was partway between its investigation of active sand dunes lower on Mount Sharp, and Vera Rubin Ridge, a destination uphill where the rover team intends to examine outcrops where hematite has been identified from Mars orbit. The rover's surroundings include tan rocks and patches of dark sand. As in previous HiRISE color images of Curiosity since the rover was at its landing site, the rover ap
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Geologic layering on Mars hints at past conditions. This image from the HI RISE high-resolution camera on board the Mars Reconnaissance Orbiter (MRO) shows multiple layers of exposed sedimentary rock on Mars in a region known as Arabia Terra. Referred to as cyclic bedding” by geologists, this pattern of layering is caused by repeated fluctuations in the amount of sediment available to create new rock layers. This is often caused by long-term changes in the climate of a region, or even by wobbles in a planet’s rotation which can make certain areas experience long periods of dry climate followed by periods of wetter climate. If this is the case with these particular landforms on Mars, it may point to repeatedly wetter times in the red planet’s past. The layers seen in this image are up to 30 feet thick in places and have been deposited over tens of millions of years. The colour is not true colour but rather indicates different textures of material.
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This inner slope of a crater on southern Mars has several of the seasonal dark streaks called recurrent slope lineae, or RSL, that a November 2017 report interprets as granular flows, rather than darkening due to flowing water. This 2011 view near the top of the southern rim of Tivat Crater comes from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. North is toward the top and the slope descends toward the northwest. The view spans an area about 1,000 feet (300 meters) wide. Figure 1 includes a scale bar of 50 meters (164 feet). HiRISE began viewing Mars in 2006. Multiple observations of some sites resulted in discovery of RSL in 2011 and has confirmed many thousands of them at more than 50 sites, from equatorial to mid-latitude north and south. These narrow, dark features appear in warm seasons, gradually extend downslope, fade away in winter and reappear the next year. On Earth, only seeping water is known to have these behaviors.
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Aerial view of geometric shapes geoglyph in Nazca, Peru.
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Plains and Impact Crater on Venus Seen by Magellan (Digitally Generated)
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Natural Science, Structure of surface of the stone,
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Small impact craters retain their original bowl shape, but once a crater is large enough that the force of gravity on the slopes of the crater wall is greater than the strength of the target material, the wall collapses inward to form a central peak.
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This April 6, 2014, image from NASA's Mars Reconnaissance Orbiter shows numerous landslides in the vicinity of where an impact crater was excavated in March 2012.
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This observation from NASA's Mars Reconnaissance Orbiter shows the nature of large fissures in a smooth apron around a mound in the Phlegra region.
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This image from NASA's Mars Reconnaissance Orbiter reveals layers filling a larger crater, perhaps a combination of lava, impact ejecta, and sediments.
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This image captured by NASA's Mars Reconnaissance Orbiter, shows the floor of Suzhi Crater, an approximately 25-kilometer diameter impact crater located northeast of Hellas Planitia.
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This false color image from NASA's Magellan spacecraft shows a portion of Bereghinya Planitia (plains) in the northern hemisphere of Venus.
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ISS017-E-013025 (12 Aug. 2008) --- The Tifernine Dune Field in Algeria is featured in this image photographed by an Expedition 17 crewmember on the International Space Station. The Tifernine Dune Field is located at the southernmost tip of the Grand Erg Oriental, a "dune sea" that occupies a large portion of the Sahara Desert in eastern Algeria. This view illustrates the interface between the yellow-orange sand dunes of the field and adjacent dark brown consolidated rocks of the Tinrhert Plateau to the south and east (right). NASA scientists point out that three distinct landform types are visible in the image, each providing information about past and present climate in the area. The oldest landform is represented by the rocks of the Tinrhert Plateau, which are characterized by a number of incised channels in the bedrock -- these formed during a wet and cool climate period, most probably by glacial meltwater streams. As the present dry and hot climate that characterizes the Sahara bec
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Complicated Lava Cooling. This HiRISE image shows a classic example of platy-ridged lava. Scientists think that this is the same as a lava type called rubbly pahoehoe on Earth. In this lava, a crust of rubble forms as the lava partially cools but then tears up its own cover. Eventually, the rubble can form plates that can be rafted apart as the lava cools further, producing textures like those visible on terrestrial lava lakes that have cooled. We see here a complex history of these processes. There are two different shapes of the rubble (at right, and top left/bottom center) indicating two stages of formation. The smooth area at center also is divided into two domains with different polygon styles, indicating that the rift opened, partially cooled, and then opened further. https //photojournal.jpl.nasa.gov/catalog/PIA25948
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Image Number: 6145-45128224Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Underground Testing and MiningContributor:PiemagsModel Release:NoProperty Release:NoResolution:2880×1800
Mars
Mars Reconnaissance Orbiter (MRO)|