Astronomy:Common surface features of Mars
The common surface features of Mars include dark slope streaks, dust devil tracks, sand dunes, Medusae Fossae Formation, fretted terrain, layers, gullies, glaciers, scalloped topography, chaos terrain, possible ancient rivers, pedestal craters, brain terrain, and ring mold craters.
A new phenomenon known as slope streaks has been uncovered by the HiRISE camera on the Mars Reconnaissance Orbiter. These features appear on crater walls and other slopes, and they are thin and many hundreds of metres long. The streaks have been observed to grow slowly over the course of a year or so, always beginning at a point source. Newly formed streaks are dark in colour but fade as they age until white. The cause is unknown, but theories range from dry dust avalanches (the favoured theory) to brine seepage.
Examples of dark slope streaks from various parts of Mars are shown below. Click on image to get a better view.
Tikonravev Crater floor in Arabia quadrangle, as seen by Mars Global Surveyor. Click on image to see dark slope streaks and layers.
Close-up of some layers under cap rock of a pedestal crater and a dark slope streak, as seen by HiRISE under HiWish program.
Dark slope streaks on mesa, as seen by HiRISE under HiWish program Location is Amazonis quadrangle.
Recurrent slope lineae
Dust devil tracks
Many areas on Mars experience the passage of giant dust devils. A thin coating of fine bright dust covers most of the Martian surface. When a dust devil travels by, it blows away the coating and exposes the underlying dark surface. These dust devils have been seen both from the ground and from orbit. They have even blown the dust off the solar panels of the Spirit and Opportunity Rovers on Mars, greatly extending their lives. The twin Rovers were designed to last for 3 months; instead, Spirit lasted for 6 years, 77 days, while Opportunity continued to operate for a staggering 14 years, 136 days. The pattern of the tracks have been shown to change every few months.
Pattern of large and small tracks made by giant dust devils, as seen by under the MOC Public Targeting Program
Dust devil tracks, as seen by HiRISE under HiWish program
Many places on Mars show rocks arranged in layers. Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers. A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars. Layers can be hardened by the action of groundwater. Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through. When ground water surfaces in low areas containing sediments, water evaporates in the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together.
Layers in Firsoff Crater, as seen by HiRISE under HiWish program Note: this image field can be found in the previous image of the layers in Firsoff Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
Light toned butte on floor of crater, as seen by HiRISE under HiWish program. Arrows show outcrops of light toned material. Light toned material is probably sulfate-rich and similar to material examined by Spirit Rover, and it once probably covered the whole floor. Other images below show enlargements of the butte. Location is Margaritifer Sinus quadrangle.
Layered terrain in Aeolis quadrangle, as seen by HiRISE under HiWish program.
Wide view of layered terrain, as seen by HiRISE under HiWish program Location is northeast of Gale Crater in Aeolis quadrangle.
Butte in Crommelin Crater, as seen by HiRISE under HiWish program. Location is Oxia Palus quadrangle.
Layers in Crommelin Crater, as seen by HiRISE under HiWish program. Location is Oxia Palus quadrangle.
Layers in Crommelin Crater, as seen by HiRISE under HiWish program. Arrow indicates fault. Location is Oxia Palus quadrangle.
Layers, as seen by HiRISE under HiWish program Location is Tempe Terra
Layers, as seen by HiRISE under HiWish program Location is Tempe Terra Note: this is an enlargement of the previous image.
Layers breaking up into boulders in Galle Crater, as seen by HiRISE under HiWish program Location is Argyre quadrangle.
Layers and gullies in Galle Crater, as seen by HiRISE under HiWish program Location is Argyre quadrangle.
Layered mesa in mound in Galle Crater, as seen by HiRISE under HiWish program Location is Argyre quadrangle.
Layers and polygons in mound in Galle Crater, as seen by HiRISE under HiWish program Location is Argyre quadrangle.
Close view of layers in mound in Galle Crater, as seen by HiRISE under HiWish program Location is Argyre quadrangle.
Close view of layers, as seen by HiRISE under HiWish program Location is Arabia quadrangle.
Layers in Ice Cap
Layers exposed in northern ice cap, as seen by HiRISE under HiWish program
Many locations on Mars have sand dunes. An erg (or sand sea), made up of aeolian dune fields referred to as the Circumpolar Dune Field surrounds most of the north polar cap. The dunes are covered by a seasonal carbon dioxide frost that forms in early autumn and remains until late spring. Many martian dunes strongly resemble terrestrial dunes but images acquired by the High-Resolution Imaging Science Experiment on the Mars Reconnaissance Orbiter have shown that martian dunes in the north polar region are subject to modification via grainflow triggered by seasonal CO
2 sublimation, a process not seen on Earth. Many dunes are black because they are derived from the dark volcanic rock basalt. Extraterrestrial sand seas such as those found on Mars are referred to as "undae" from the Latin for waves.
Dark dunes (probably basalt) which form a dark spot in Noachis. Picture from Mars Global Surveyor.
Dunes, as seen by HiRISE under HiWish program. Location is Eridania quadrangle.
Dunes in Mare Tyrrhenum quadrangle, as seen by HiRISE under HiWish program
Close view of dunes Mare Tyrrhenum quadrangle, as seen by HiRISE under HiWish program
Close, color view of dunes Mare Tyrrhenum quadrangle, as seen by HiRISE under HiWish program Ripples are visible on dune surface.
Martian gullies are small, incised networks of narrow channels and their associated downslope sediment deposits, found on the planet of Mars. They are named for their resemblance to terrestrial gullies. First discovered on images from Mars Global Surveyor, they occur on steep slopes, especially on the walls of craters. Usually, each gully has a dendritic alcove at its head, a fan-shaped apron at its base, and a single thread of incised channel linking the two, giving the whole gully an hourglass shape. They are believed to be relatively young because they have few, if any craters.
On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research.
Gullies near Newton Crater, as seen by HiRISE under the HiWish Program. Location is the Phaethontis quadrangle.
Close-up of gully showing multiple channels and patterned ground, as seen by HiRISE under the HiWish program. Location is the Phaethontis quadrangle.
Group of gullies in Thaumasia quadrangle, as seen by HiRISE under the HiWish program.
Gullies and massive flow of material, as seen by HiRISE under HiWish program. Gullies are enlarged in next image. Location is Bamberg crater
Gullies in a crater, as seen by HiRISE under HiWish program. Location is in the Mare Acidalium quadrangle.
Wide view of group of gullies, as seen by HiRISE under HiWish program. Note that part of this image is enlarged in the following image. Location is Diacria quadrangle.
Close-up of gullies, as seen by HiRISE under HiWish program. Streamlined features in the channels are suggestive of a formation by running water. Location is Diacria quadrangle.
Gullies in crater in Phaethontis quadrangle, as seen by HiRISE under HiWish program
Floor of crater from previous image in Phaethontis quadrangle, as seen by HiRISE under HiWish program Ring mold crater is caused by asteroid reaching an ice layer. Pits on floor may be from ice escaping the ground.
Gullies in crater, as seen by HiRISE under HiWish program. Location is Eridania quadrangle.
Close-up of gullies in crater showing channels within larger valleys and curves in channels. These characteristics suggest they were made by flowing water. Note: this is an enlargement of the previous image by HiRISE under HiWish program. Location is Eridania quadrangle.
Close-up of gully network showing branched channels and curves; these characteristics suggest creation by a fluid. Note: this is an enlargement of a previous wide view of gullies in a crater, as seen by HiRISE under HiWish program. Location is Eridania quadrangle.
Gullies in two levels of a crater wall, as seen by HiRISE under HiWish program. Gullies at two levels suggests they were not made with an aquifer, as was first suggested. Location is Phaethontis quadrangle.
Image of gullies with main parts labeled. The main parts of a Martian gully are alcove, channel, and apron. Since there are no craters on this gully, it is thought to be rather young. Picture was taken by HiRISE under HiWish program. Location is Phaethontis quadrangle.
Close-up of gully aprons showing they are free of craters; hence very young. Location is Phaethontis quadrangle. Picture was taken by HiRISE under HiWish program.
Gullies on wall of crater, as seen by HiRISE under HiWish program Location is the Mare Acidalium quadrangle.
Close-up of gully channels, as seen by HiRISE under HiWish program. This image shows many streamlined forms and some benches along a channel. These features suggest formation by running water. Benches are usually formed when the water level goes down a bit and stays at that level for a time. Picture was taken with HiRISE under HiWish program. Location is the Mare Acidalium quadrangle. Note this is an enlargement of a previous image.
Gullies on Dunes
Gullies are found on some dunes. These are somewhat different from gullies in other places, like the walls of craters. Gullies on dunes seem to keep the same width for a long distance and often just end with a pit, instead of an apron. They are often just a few meters across with raised banks along the sides. Many of these gullies are found on dunes in Russell (Martian crater). In the winter dry ice accumulates on the dunes and then in the spring dark spots appear and dark-toned streaks grow downhill. After the dry ice is gone, new channels are visible. These gullies may be caused by blocks of dry ice moving down the steep slope or perhaps from dry ice starts the sand moving. In the thin atmosphere of mars, dry ice will expel carbon dioxide with vigor.
Close view of the end of gullies in Russell Crater, as seen by HiRISE Note: These type of gullies do not usually end with an apron. The location is Noachis quadrangle.
Medusae Fossae Formation
The Medusae Fossae Formation is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars. Sometimes the formation appears as a smooth and gently undulating surface; however, in places it is wind-sculpted into ridges and grooves. Radar imaging has suggested that the region may contain either extremely porous rock (for example volcanic ash) or deep layers of glacier-like ice deposits amounting to about the same quantity as is stored in Mars' south polar cap.
The lower portion (member) of Medusae Fossae Formation contains many patterns and shapes that are thought to be the remains of streams. It is believed that streams formed valleys that were filled and became resistant to erosion by cementation of minerals or by the gathering of a coarse covering layer. These inverted stream beds are sometimes called sinuous ridges or raised curvilinear features. They may be a kilometer or so in length. Their height ranges from a meter to greater than 10 meters, while the width of the narrow ones is less than 10 meters.
The wind has eroded the surface of the formation into a series of linear ridges called yardangs. These ridges generally point in the direction of the prevailing winds that carved them and demonstrate the erosive power of martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles, and was most likely formed by the deposition of wind-blown dust or volcanic ash. Layers are seen in parts of the formation. A resistant caprock on the top of yardangs has been observed in Viking, Mars Global Surveyor, and HiRISE photos. Very few impact craters are visible throughout the area so the surface is relatively young.
Medusae Fossae Formation as seen with Mars Odyssey's THEMIS. Notice elongated formations called yardangs.
Layers in lower member of Medusae Fossae Formation, as seen by HiRISE. Location is Aeolis quadrangle.
Yardangs are common in some regions on Mars, especially in the Medusae Fossae Formation of the Amazonis quadrangle and near the equator. They are formed by the action of wind on sand sized particles; hence they often point in the direction that the winds were blowing when they were formed. Because they exhibit very few impact craters they are believed to be relatively young.
Yardangs, as seen by HiRISE under HiWish program Location is near Gordii Dorsum in the Amazonis quadrangle. These yardangs are in the upper member of the Medusae Fossae Formation.
Fretted terrain is a type of surface feature common to certain areas of Mars and discovered in Mariner 9 images. It lies between two different surfaces. The surface of Mars can be divided into two parts: low, young, uncratered plains that cover most of the northern hemisphere, and high-standing, old, heavily cratered areas that cover the southern hemisphere and a small part of the northern hemisphere. Between these two zones is the fretted terrain, containing a complicated mix of cliffs, mesas, buttes, and straight-walled and sinuous canyons. Fretted terrain contains smooth, flat lowlands along with steep cliffs. The scarps or cliffs are usually 1 to 2 km high. Channels in the area have wide, flat floors and steep walls. Fretted terrain is most common in northern Arabia, between latitudes 30°N and 50°N and longitudes 270°W and 360°W. Parts of the fretted terrain are called Deuteronilus Mensae and Protonilus Mensae.
In fretted terrain, the land seems to transition from narrow straight valleys to isolated mesas. Most of the mesas are surrounded by forms that have been called a variety of names (circum-mesa aprons, debris aprons, rock glaciers, and lobate debris aprons). At first they appeared to resemble rock glaciers on Earth, but scientists could not be sure. Eventually, proof of their true nature was discovered by radar studies with the Mars Reconnaissance Orbiter and showed that they contain pure water ice covered with a thin layer of rocks that insulated the ice.
In addition to rock covered glaciers around mesas, the region has many steep-walled valleys with lineations—ridges and grooves—on their floors. The material comprising these valley floors is called lineated valley fill. In some of the best images taken by the Viking Orbiters, some of the valley fill appeared to resemble alpine glaciers on Earth. Given this similarity, some scientists assumed that the lineations on these valley floors might have formed by flow of ice in (and perhaps through) these canyons and valleys. Today, it is generally agreed that glacial flow caused the lineations.
Fretted terrain of Ismenius Lacus showing flat floored valleys and cliffs. Photo taken with Mars Orbiter Camera (MOC)on the Mars Global Surveyor.
Enlargement of the photo on the left showing cliff. Photo taken with high resolution camera of Mars Global Surveyor (MGS).
The arrow in the left picture points to a possibly valley carved by a glacier. The image on the right shows the valley greatly enlarged in a Mars Global Surveyor image.
Wide view of mesa with CTX showing Cliff face and location of lobate debris apron (LDA). Location is Ismenius Lacus quadrangle.
Enlargement of previous CTX image of mesa This image shows the cliff face and detail in the LDA. Image taken with HiRISE under HiWish program. Location is Ismenius Lacus quadrangle.
Wide CTX view showing mesa and buttes with lobate debris aprons and lineated valley fill around them. Location is Ismenius Lacus quadrangle.
Close-up of lineated valley fill (LVF), as seen by HiRISE under HiWish program Note: this is an enlargement of the previous CTX image.
Glaciers, loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past.
Glacier as seen by HiRISE under the HiWish program. Area in rectangle is enlarged in the next photo. Zone of accumulation of snow at the top. Glacier is moving down valley, then spreading out on plain. Evidence for flow comes from the many lines on surface. Location is in Protonilus Mensae in Ismenius Lacus quadrangle.
Enlargement of area in rectangle of the previous image. On Earth the ridge would be called the terminal moraine of an alpine glacier. Picture taken with HiRISE under the HiWish program. Image from Ismenius Lacus quadrangle.
Glacier coming out of valley, as seen by HiRISE under HiWish program Location is rim of Moreux Crater. Location is Ismenius Lacus quadrangle.
Probable glacier as seen by HiRISE under HiWish program. Radar studies have found that it is made up of almost totally of pure ice. It appears to be moving from the high ground (a mesa) on the right. Location is Ismenius Lacus quadrangle.
Lobate debris aprons (LDAs) around a mesa, as seen by CTX. Mesa and LDAs are labeled so one can see their relationship. Radar studies have determined that LDAs contain ice; therefore, these can be important for future colonists of Mars. Location is Ismenius Lacus quadrangle.
Wide CTX view of mesa showing lobate debris apron (LDA) and lineated valley fill. Both are believed to be debris covered glaciers. Location is Ismenius Lacus quadrangle.
Close-up of lobate debris apron from the previous CTX image of a mesa. Image shows open-cell brain terrain and closed-cell brain terrain, which is more common. Open-cell brain terrain is thought to hold a core of ice. Image is from HiRISE under HiWish program.
Concentric crater fill
Concentric crater fill, like lobate debris aprons and lineated valley fill, is believed to be ice-rich. Based on accurate topography measures of height at different points in these craters and calculations of how deep the craters should be based on their diameters, it is thought that the craters are 80% filled with mostly ice. That is, they hold hundreds of meters of material that probably consists of ice with a few tens of meters of surface debris. The ice accumulated in the crater from snowfall in previous climates. Recent modeling suggests that concentric crater fill develops over many cycles in which snow is deposited, then moves into the crater. Once inside the crater, shade and dust preserve the snow. The snow changes to ice. The many concentric lines are created by the many cycles of snow accumulation. Generally snow accumulates whenever the axial tilt reaches 35 degrees.
Close-up view of concentric crater fill, as seen by HiRISE under HiWish program Note: this is an enlargement of previous image of a concentric crater. Location is Phaethontis quadrangle.
Well-developed hollows, as seen by HiRISE under the HiWish program. Location is the Casius quadrangle. Note: this is an enlargement of the previous image that was taken by CTX.
Wide view of Buttes and Mesas, as seen by HiRISE under HiWish program Location is Elysium quadrangle.
Layers in mesa, as seen by HiRISE under HiWish program Location is Mare Acidalium quadrangle.
Wide view of layered buttes and small mesas, as seen by HiRISE under HiWish program Some dark slope streaks are visible. Location is Aeolis quadrangle. Note: Parts of this image are enlarged in next three pictures.
Chaos terrain is believed to be associated with the release of huge amounts of water. The chaotic features may have collapsed when water came out of the surface. Martian outflow channels commonly begin with a Chaos region. A chaotic region can be recognized by a tangle of mesas, buttes, and hills, all chopped through with valleys which in places look almost patterned. Some parts of this chaotic area have not collapsed completely—they are still formed into large mesas, so they may still contain water ice. Chaotic terrain occurs in numerous locations on Mars, and always gives the strong impression that something abruptly disturbed the ground. Chaos regions formed long ago. By counting craters (more craters in any given area means an older surface) and by studying the valleys' relations with other geological features, scientists have concluded the channels formed 2.0 to 3.8 billion years ago.
Aureum Chaos, as seen by HiRISE, under the HiWish program.
Wide view of layers in wall of Aurorae Chaos, as seen by HiRISE under HiWish program
Remnants of a 50–100 meter thick mantling, called the upper plains unit, has been discovered in the mid-latitudes of Mars. First investigated in the Deuteronilus Mensae region, but it occurs in other places as well. The remnants consist of sets of dipping layers in craters and along mesas. Sets of dipping layers may be of various sizes and shapes—some look like Aztec pyramids from Central America.
Wide view of dipping layers along mesa walls, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Close view of dipping layers along a mesa wall, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
This unit also degrades into brain terrain. Brain terrain is a region of maze-like ridges 3–5 meters high. Some ridges may consist of an ice core, so they may be sources of water for future colonists.
Brain terrain, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Some regions of the upper plains unit display large fractures and troughs with raised rims; such regions are called ribbed upper plains. Fractures are believed to have started with small cracks from stresses. Stress is suggested to initiate the fracture process since ribbed upper plains are common when debris aprons come together or near the edge of debris aprons—such sites would generate compressional stresses. Cracks exposed more surfaces, and consequently more ice in the material sublimates into the planet's thin atmosphere. Eventually, small cracks become large canyons or troughs. Small cracks often contain small pits and chains of pits; these are thought to be from sublimation of ice in the ground. Large areas of the Martian surface are loaded with ice that is protected by a meters thick layer of dust and other material. However, if cracks appear, a fresh surface will expose ice to the thin atmosphere. In a short time, the ice will disappear into the cold, thin atmosphere in a process called sublimation. Dry ice behaves in a similar fashion on the Earth. On Mars sublimation has been observed when the Phoenix lander uncovered chunks of ice that disappeared in a few days. In addition, HiRISE has seen fresh craters with ice at the bottom. After a time, HiRISE saw the ice deposit disappear.
Die-sized clumps of bright material in the enlarged "Dodo-Goldilocks" trench vanished over the course of four days, implying that they were composed of ice which sublimated following exposure.
The upper plains unit is thought to have fallen from the sky. It drapes various surfaces, as if it fell evenly. As is the case for other mantle deposits, the upper plains unit has layers, is fine-grained, and is ice-rich. It is widespread; it does not seem to have a point source. The surface appearance of some regions of Mars is due to how this unit has degraded. It is a major cause of the surface appearance of lobate debris aprons. The layering of the upper plains mantling unit and other mantling units are believed to be caused by major changes in the planet's climate. Models predict that the obliquity or tilt of the rotational axis has varied from its present 25 degrees to maybe over 80 degrees over geological time. Periods of high tilt will cause the ice in the polar caps to be redistributed and change the amount of dust in the atmosphere.
Much of the Martian surface is covered with a thick ice-rich, mantle layer that has fallen from the sky a number of times in the past. In some places a number of layers are visible in the mantle.
Mantle layers, as seen by HiRISE under HiWish program. Location is Eridania quadrangle
Close up view of mantle, as seen by HiRISE under the HiWish program. Mantle may be composed of ice and dust that fell from the sky during past climatic conditions. Location is Cebrenia quadrangle.
Smooth mantle with layers in Hellas quadrangle, as seen by HiRISE under HiWish program
Close view of mantle, as seen by HiRISE under HiWish program Arrows show craters along edge which highlight the thickness of mantle. Location is Ismenius Lacus quadrangle.
Close view that displays the thickness of the mantle, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
It fell as snow and ice-coated dust. There is good evidence that this mantle is ice-rich. The shapes of the polygons common on many surfaces suggest ice-rich soil. High levels of hydrogen (probably from water) have been found with Mars Odyssey. Thermal measurements from orbit suggest ice. The Phoenix Lander found water ice directly since it landed in a field of polygons and its landing rockets exposed a pure ice surface. Theory had predicted that ice would be found under a few cm of soil. This mantle layer is called "latitude dependent mantle" because its occurrence is related to the latitude. It is this mantle that cracks and then forms polygonal ground. This cracking of ice-rich ground is predicted based on physical processes. 
Polygonal, patterned ground is quite common in some regions of Mars. It is commonly believed to be caused by the sublimation of ice from the ground. Sublimation is the direct change of solid ice to a gas. This is similar to what happens to dry ice on the Earth. Places on Mars that display polygonal ground may indicate where future colonists can find water ice. Patterned ground forms in a mantle layer, called latitude dependent mantle, that fell from the sky when the climate was different.
High center polygons, shown with arrows, as seen by HiRISE under HiWish program. Location is Casius quadrangle. Image enlarged with HiView.
Scalloped terrain labeled with both low center polygons and high center polygons, as seen by HiRISE under HiWish program Location is Casius quadrangle. Image enlarged with HiView.
High and low center polygons, as seen by HiRISE under HiWish program Location is Casius quadrangle. Image enlarged with HiView.
Close-up of high center polygons seen by HiRISE under HiWish program Troughs between polygons are easily visible in this view. Location is Ismenius Lacus quadrangle.
Scalloped topography is common in the mid-latitudes of Mars, between 45° and 60° north and south. It is particularly prominent in the region of Utopia Planitia in the northern hemisphere and in the region of Peneus and Amphitrites Patera in the southern hemisphere. Such topography consists of shallow, rimless depressions with scalloped edges, commonly referred to as "scalloped depressions" or simply "scallops". Scalloped depressions can be isolated or clustered and sometimes seem to coalesce. A typical scalloped depression displays a gentle equator-facing slope and a steeper pole-facing scarp. This topographic asymmetry is probably due to differences in insolation. Scalloped depressions are believed to form from the removal of subsurface material, possibly interstitial ice, by sublimation. This process may still be happening at present.
On November 22, 2016, NASA reported finding a large amount of underground ice in the Utopia Planitia region of Mars. The volume of water detected has been estimated to be equivalent to the volume of water in Lake Superior. The volume of water ice in the region were based on measurements from the ground-penetrating radar instrument on Mars Reconnaissance Orbiter, called SHARAD. From the data obtained from SHARAD, “dielectric permittivity”, or the dielectric constant was determined. The dielectric constant value was consistent with a large concentration of water ice.
Stages in scallop formation, as seen by HiRISE. Location is Hellas quadrangle.
There is great deal of evidence that water once flowed in river valleys on Mars. Pictures from orbit show winding valleys, branched valleys, and even meanders with oxbow lakes. Some are visible in the pictures below.
Channel in Arabia, as seen by HiRISE under HiWish program. This is an enlargement of the previous image that was taken with CTX to give a wide view.
Oxbow lake, as seen by HiRISE under HiWish program.
Channel showing an old oxbow and a cutoff, as seen by HiRISE under HiWish program. Location is Memnonia quadrangle.
Channel, as seen by HiRISE under HiWish program Location is the Cebrenia quadrangle.
Streamlined shapes represent more evidence of past flowing water on Mars. Water shaped features into streamlined shapes.
Streamlined feature, as seen by HiRISE under HiWish program Location is Memnonia quadrangle.
Wide view of streamlined shapes in Amenthes quadrangle, as seen by HiRISE under HiWish program
Streamlined shapes, as seen by HiRISE under HiWish program Location is the Elysium quadrangle.
Wide view of a delta in Holden Crater, as seen by CTX
Pedestal craters are believed to be caused by a crater's ejecta protecting the material beneath it from eroding. The underlying material is probably ice-rich; hence these craters indicate where and how much ice was present in the ground.
Drawing shows a later idea of how some pedestal craters form. In this way of thinking, an impacting projectile goes into an ice-rich layer—but no further. Heat and wind from the impact hardens the surface against erosion. This hardening can be accomplished by the melting of ice which produces a salt/mineral solution thereby cementing the surface.
Dark slope streaks near the top of a pedestal crater, as seen by HiRISE under the HiWish program. Note in the middle of the picture, one can see the track of a boulder that rolled down a slope.
Pedestal crater, as seen by HiRISE under HiWish program The ejecta is not symmetrical around crater because the asteroid came at a low angle out of the North East. The ejecta protected the underlying material from erosion; hence the crater looks elevated. The location is Casius quadrangle.
Close-up of East side (right side) of previous image of pedestal crater showing polygons on lobe. Since the margin of the crater has lobes and polygons, it is believed there is ice under the protective top. Picture taken with HiRISE under HiWish program. Note: this is an enlargement of the previous image.
Pedestal crater with layers, as seen by HiRISE under HiWish program Location is Amazonis quadrangle.
Pedestal crater with boulders along rim. Such craters are called "halo craters." Picture taken with HiRISE under HiWish program.
Boulders, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Boulder and boulder tracks, as seen by HiRISE under HiWish program The arrow shows a boulder that has made a track in the sand as it rolled down dune. Location is Mare Boreum quadrangle.
Boulders and tracks, as seen by HiRISE under HiWish program The arrows show a boulders that have produced a track by rolling down dune. Location is Mare Boreum quadrangle.
Brain terrain is a feature of the Martian surface, consisting of complex ridges found on lobate debris aprons, lineated valley fill and concentric crater fill. It is so named because it suggests the ridges on the surface of the human brain. Wide ridges are called closed-cell brain terrain, and the less common narrow ridges are called open-cell brain terrain. It is thought that the wide closed-cell terrain contains a core of ice, and when the ice disappears the center of the wide ridge collapses to produce the narrow ridges of the open-cell brain terrain.
Ring mold craters are believed to be formed from asteroid impacts into ground that has an underlying layer of ice. The impact produces an rebound of the ice layer to form a "ring-mold" shape.
Ring mold craters on floor of a crater, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Ring mold craters of various sizes on floor of a crater, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Rootless cones are caused by explosions of lava with ground ice under the flow. The ice melts and turns into a vapor that expands in an explosion that produces a cone or ring. Features like these are found in Iceland, when lavas cover water-saturated substrates.
Some features look like volcanoes. Some of them may be mud volcanoes where pressurized mud is forced upward forming cones. These features may be places to look for life as they bring to the surface possible life that has been protected from radiation.
Lava flow in Tharsis quadrangle, as seen by HiRISE under HiWish program
Wide view of streamlined shape and rafts of lava, as seen by HiRISE under HiWish program Location is Amazonis quadrangle.
Linear Ridge Networks
Linear ridge networks are found in various places on Mars in and around craters. Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation.
Wide view of network of ridges, as seen by HiRISE under HiWish program Portions of this image are enlarged in following images. Location is the Casius quadrangle.
Fractures forming blocks
In places large fractures break up surfaces. Sometimes straight edges are formed and large cubes are created by the fractures.
Volcanoes under ice
There is evidence that volcanoes sometimes erupt under ice, as they do on Earth at times. What seems to happen it that much ice melts, the water goes away, and then the surface cracks and collapses. These exhibit concentric fractures and large pieces of ground that seemed to have been pulled apart. Sites like this may have recently had held liquid water, hence they may be fruitful places to search for evidence of life.
In the spring, various shapes appear because frost is disappearing from the surface, exposing the underling dark soil. Also, in some places dust is blown out of in geyser-like eruptions that are sometimes called "spiders." If a wind is blowing, the material creates a long, dark streak or fan.
During the winter, much frost accumulates. It freezes out directly onto the surface of the permanent polar cap, which is made of water ice covered with layers of dust and sand. The deposit begins as a layer of dusty CO
2 frost. Over the winter, it recrystallizes and becomes denser. The dust and sand particles caught in the frost slowly sink. By the time temperatures rise in the spring, the frost layer has become a slab of semi-transparent ice about 3 feet thick, lying on a substrate of dark sand and dust. This dark material absorbs light and causes the ice to sublimate (turn directly into a gas). Eventually much gas accumulates and becomes pressurized. When it finds a weak spot, the gas escapes and blows out the dust. Speeds can reach 100 miles per hour. Dark channels can sometimes be seen; they are called "spiders." The surface appears covered with dark spots when this process is occurring.
- Astronomy:Chaos terrain – Distinctive area of broken or jumbled terrain
- Astronomy:Climate of Mars – Climate patterns of the terrestrial planet
- Astronomy:Dark slope streak – Surface feature of Mars
- Astronomy:Dust devil tracks
- Astronomy:Fretted terrain – Surface feature common to certain areas of Mars
- Astronomy:Geology of Mars – Scientific study of the surface, crust, and interior of the planet Mars
- Astronomy:Geysers on Mars – Putative CO2 gas and dust eruptions on Mars
- Earth:Glacier – Persistent body of ice that is moving under its own weight
- Astronomy:Glaciers on Mars – Extraterrestrial bodies of ice
- Astronomy:Groundwater on Mars – Water held in permeable ground
- Astronomy:Ismenius Lacus quadrangle – Map of Mars
- Astronomy:Lineated valley fill – Martian geologic feature
- Astronomy:Martian chaos terrain – Irregular groups of large blocks of rock
- Martian gullies – Incised networks of narrow channels and sediments on Mars
- Astronomy:Seasonal flows on warm Martian slopes – Surface features on Mars—recurrent slope lineae
- Astronomy:Scalloped topography – Depressions in topography at mid-latitudes of Mars
- Astronomy:Water on Mars – Study of past and present water on Mars
- Astronomy:Yardangs on Mars
- "Newly-Formed Slope Streaks". NASA. http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_002396_1900.
- McEwen, A. (2014). "Recurring slope lineae in equatorial regions of Mars". Nature Geoscience 7 (1): 53–58. doi:10.1038/ngeo2014. Bibcode: 2014NatGe...7...53M.
- Ojha, L. (2014). "HiRISE observations of Recurring Slope Lineae (RSL) during southern summer on Mars". Icarus 231: 365–376. doi:10.1016/j.icarus.2013.12.021. Bibcode: 2014Icar..231..365O.
- McEwen, A. (2011). "Seasonal Flows on Warm Martian Slopes". Science 333 (6043): 740–743. doi:10.1126/science.1204816. PMID 21817049. Bibcode: 2011Sci...333..740M.
- recurring slope lineae | Red Planet Report
- "Mars Exploration Rover Mission: Press Release Images: Spirit". Marsrovers.jpl.nasa.gov. http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412a.html.
- "Ken Edgett". NASA's Mars Exploration Program. http://mars.jpl.nasa.gov/spotlight/KenEdgett.html.
- "HiRISE | High Resolution Imaging Science Experiment". Hirise.lpl.arizona.edu?psp_008437_1750. http://hirise.lpl.arizona.edu?PSP_008437_1750.
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
- Massé, M.; Bourgeois, O (March 2011). "Distribution and Origin of Polar Gypsum on Mars". 42nd Lunar and Planetary Science Conference. Lunar and Planetary Institute. http://www.lpi.usra.edu/meetings/lpsc2011/pdf/1737.pdf.
- Schatz, Volker; H. Tsoar; K. S. Edgett; E. J. R. Parteli; H. J. Herrmann (2006). "Evidence for indurated sand dunes in the Martian north polar region". Journal of Geophysical Research 111 (E04006): E04006. doi:10.1029/2005JE002514. Bibcode: 2006JGRE..111.4006S.
- Hansen, C. J.; Bourke, M.; Bridges, N. T.; Byrne, S.; Colon, C.; Diniega, S.; Dundas, C.; Herkenhoff, K. et al. (4 February 2011). "Seasonal Erosion and Restoration of Mars' Northern Polar Dunes". Science 331 (6017): 575–578. doi:10.1126/science.1197636. PMID 21292976. Bibcode: 2011Sci...331..575H. http://www.lpl.arizona.edu/~shane/publications/hansen_etal_science_2011.pdf. Retrieved 2015-02-20.
- Malin, M.; Edgett, K. (2000). "Evidence for recent groundwater seepage and surface runoff on Mars". Science 288 (5475): 2330–2335. doi:10.1126/science.288.5475.2330. PMID 10875910. Bibcode: 2000Sci...288.2330M.
- "Linear Gullies on Mars Caused by Sliding Dry-Ice". 12 June 2013. https://scitechdaily.com/linear-gullies-on-mars-caused-by-sliding-dry-ice/.
- Dundas, C., et al. 2012. Seasonal activity and morphological changes in martian gullies. Icarus: 220, 124–143.
- McEwen, A., et al. 2017. Mars The Pristine Beauty of the Red Planet. University of Arizona Press. Tucson.
- Fraser Cain (2005-03-29). "Medusa Fossae Region on Mars". Universetoday.com. http://www.universetoday.com/2005/03/29/medusa-fossae-region-on-mars/.
- Shiga, David (1 November 2007). "Vast amount of water ice may lie on Martian equator". New Scientist Space. https://www.newscientist.com/article/dn12866-vast-amount-of-water-ice-may-lie-on-martian-equator.html.
- Watters, T. R.; Campbell, B.; Carter, L.; Leuschen, C. J.; Plaut, J. J.; Picardi, G.; Orosei, R.; Safaeinili, A. et al. (2007). "Radar Sounding of the Medusae Fossae Formation Mars: Equatorial Ice or Dry, Low-Density Deposits?". Science 318 (5853): 1125–8. doi:10.1126/science.1148112. PMID 17975034. Bibcode: 2007Sci...318.1125W.
- Zimbelman, James R.; Griffin, Lora J. (2010). "HiRISE images of yardangs and sinuous ridges in the lower member of the Medusae Fossae Formation, Mars". Icarus 205 (1): 198–210. doi:10.1016/j.icarus.2009.04.003. Bibcode: 2010Icar..205..198Z.
- Scott, David H.; Tanaka, Kenneth L. (1982). "Ignimbrites of Amazonis Planitia Region of Mars". Journal of Geophysical Research 87 (B2): 1179–1190. doi:10.1029/JB087iB02p01179. Bibcode: 1982JGR....87.1179S.
- Malin, MC; Carr, MH; Danielson, GE; Davies, ME; Hartmann, WK; Ingersoll, AP; James, PB; Masursky, H et al. (March 1998). "Early views of the martian surface from the Mars Orbiter Camera of Mars Global Surveyor". Science 279 (5357): 1681–5. doi:10.1126/science.279.5357.1681. PMID 9497280. Bibcode: 1998Sci...279.1681M.
- Mandt, Kathleen E.; De Silva, Shanaka L.; Zimbelman, James R.; Crown, David A. (2008). "The origin of the Medusae Fossae Formation, Mars: Insights from a synoptic approach". Journal of Geophysical Research 113 (E12): 12011. doi:10.1029/2008JE003076. Bibcode: 2008JGRE..11312011M.
- Medusae Fossae Formation | Mars Odyssey Mission THEMIS
- SAO/NASA ADS Astronomy Abstract Service: Yardangs on Mars
- ESA - 'Yardangs' on Mars
- Strom, R.G.; Croft, S.K.; Barlow, N.G. (1992). "The Martian Impact Cratering Record". in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W. et al.. Mars. Tucson: University of Arizona Press. pp. 384–385. ISBN 978-0-8165-1257-7. https://archive.org/details/mars0000unse/page/384.
- "Catalog Page for PIA01502". Photojournal.jpl.nasa.gov. http://photojournal.jpl.nasa.gov/catalog/PIA01502.
- http://www.lpi.usra.edu/meetings/lpsc2000/pdf/1053.pdf Template:Bare URL PDF
- Head, J. et al. (2005). "Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars". Nature 434 (7031): 346–50. doi:10.1038/nature03359. PMID 15772652. Bibcode: 2005Natur.434..346H.
- Plaut, J. (2008). "Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars". Lunar and Planetary Science XXXIX: 2290.
- Holt, J. (2008). "Radar Sounding Evidence for Ice within Lobate Debris Aprons near Hellas Basin, Mid-Southern Latitudes of Mars". Lunar and Planetary Science XXXIX (1391): 2441. Bibcode: 2008LPI....39.2441H.
- Plaut Jeffrey J. et al. (28 January 2009). "Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars". Geophysical Research Letters 36 (2): L02203. doi:10.1029/2008GL036379. Bibcode: 2009GeoRL..3602203P. http://www.planetary.brown.edu/pdfs/3733.pdf.
- "Mars' climate in flux: Mid-latitude glaciers | Mars Today – Your Daily Source of Mars News". Mars Today. http://www.marstoday.com/news/viewpr.html?pid=18050.
- "Glaciers Reveal Martian Climate Has Been Recently Active". Providence, RI: Brown University. April 23, 2008. http://news.brown.edu/pressreleases/2008/04/martian-glaciers.
- "The Surface of Mars" Series: Cambridge Planetary Science (No. 6) ISBN:978-0-511-26688-1 Michael H. Carr, United States Geological Survey, Menlo Park
- Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. https://books.google.com/books?id=NoDvAAAAMAAJ. Retrieved March 7, 2011.
- Levy, J. (2009). "Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial processes". Icarus 202 (2): 462–476. doi:10.1016/j.icarus.2009.02.018. Bibcode: 2009Icar..202..462L.
- Levy, J.; Head, J.; Marchant, D. (2010). "Concentric Crater fill in the northern mid-latitudes of Mars: Formation process and relationships to similar landforms of glacial origin". Icarus 209 (2): 390–404. doi:10.1016/j.icarus.2010.03.036. Bibcode: 2010Icar..209..390L.
- Levy, J.; Head, J.; Dickson, J.; Fassett, C.; Morgan, G.; Schon, S. (2010). "Identification of gully debris flow deposits in Protonilus Mensae, Mars: Characterization of a water-bearing, energetic gully-forming process". Earth Planet. Sci. Lett. 294 (3–4): 368–377. doi:10.1016/j.epsl.2009.08.002. Bibcode: 2010E&PSL.294..368L.
- HiRISE | Ice Deposition and Loss in an Impact Crater in Utopia Basin (ESP_032569_2225)
- Garvin, J., S. Sakimoto, J. Frawley. 2003. Craters on Mars: Geometric properties from gridded MOLA topography. In: Sixth International Conference on Mars. July 20–25, 2003, Pasadena, California. Abstract 3277.
- Garvin, J. et al. 2002. Global geometric properties of martian impact craters. Lunar Planet. Sci: 33. Abstract # 1255.
- Catalog Page for PIA09662
- Kreslavsky, M. and J. Head. 2006. Modification of impact craters in the northern planes of Mars: Implications for the Amazonian climate history. Meteorit. Planet. Sci.: 41. 1633–1646
- Madeleine, J. et al. 2007. Exploring the northern mid-latitude glaciation with a general circulation model. In: Seventh International Conference on Mars. Abstract 3096.
- HiRISE | Dissected Mantled Terrain (PSP_002917_2175)
- Fastook, J., J. Head. 2014. Concentric crater fill: Rates of glacial accumulation, infilling and deglaciation in the Amazonian and Noachian of Mars. 45th Lunar and Planetary Science Conference (2014) 1227.pdf
- "Unraveling the Chaos of Aram | Mars Odyssey Mission THEMIS". Themis.asu.edu. http://themis.asu.edu/features/aramchaos.
- "Feature Image: Volcanism and Collapse in Hydraotes". 2008-11-26. http://themis.asu.edu/features/hydraotes.
- Carr, M. 2001.
- Morgenstern, A., et al. 2007
- Baker, D.; Head, J. (2015). "Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation". Icarus 260: 269–288. doi:10.1016/j.icarus.2015.06.036. Bibcode: 2015Icar..260..269B.
- Mangold, N (2003). "Geomorphic analysis of lobate debris aprons on Mars at Mars Orbiter Camera scale: Evidence for ice sublimation initiated by fractures". J. Geophys. Res. 108 (E4): 8021. doi:10.1029/2002je001885. Bibcode: 2003JGRE..108.8021M.
- Levy, J. et al. 2009. Concentric
- Bright Chunks at Phoenix Lander's Mars Site Must Have Been Ice – Official NASA press release (19.06.2008)
- Byrne, S. (2009). "Distribution of Mid-Latitude Ground Ice on Mars from New Impact Craters". Science 325 (5948): 1674–1676. doi:10.1126/science.1175307. PMID 19779195. Bibcode: 2009Sci...325.1674B.
- Head, J. et al. 2003.
- Madeleine, et al. 2014.
- Schon (2009). "A recent ice age on Mars: Evidence for climate oscillations from regional layering in mid-latitude mantling deposits". Geophys. Res. Lett. 36 (15): L15202. doi:10.1029/2009GL038554. Bibcode: 2009GeoRL..3615202S.
- Hecht, M (2002). "Metastability of water on Mars". Icarus 156 (2): 373–386. doi:10.1006/icar.2001.6794. Bibcode: 2002Icar..156..373H.
- Mustard, J. (2001). "Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice". Nature 412 (6845): 411–414. doi:10.1038/35086515. PMID 11473309. Bibcode: 2001Natur.412..411M.
- Pollack, J.; Colburn, D.; Flaser, F.; Kahn, R.; Carson, C.; Pidek, D. (1979). "Properties and effects of dust suspended in the martian atmosphere". J. Geophys. Res. 84: 2929–2945. doi:10.1029/jb084ib06p02929. Bibcode: 1979JGR....84.2929P.
- Boynton, W. (2002). "Distribution of hydrogen in the nearsurface of Mars: Evidence for sub-surface ice deposits". Science 297 (5578): 81–85. doi:10.1126/science.1073722. PMID 12040090. Bibcode: 2002Sci...297...81B.
- Kuzmin, R (2004). "Regions of potential existence of free water (ice) in the near-surface martian ground: Results from the Mars Odyssey High-Energy Neutron Detector (HEND)". Solar System Research 38 (1): 1–11. doi:10.1023/b:sols.0000015150.61420.5b. Bibcode: 2004SoSyR..38....1K.
- Mitrofanov, I. et al. 2007a. Burial depth of water ice in Mars permafrost subsurface. In: LPSC 38, Abstract #3108. Houston, TX.
- Mitrofanov, I. (2007b). "Water ice permafrost on Mars: Layering structure and subsurface distribution according to HEND/Odyssey and MOLA/MGS data". Geophys. Res. Lett. 34 (18): 18. doi:10.1029/2007GL030030. Bibcode: 2007GeoRL..3418102M.
- Mangold, N. (2004). "Spatial relationships between patterned ground and ground ice detected by the neutron spectrometer on Mars". J. Geophys. Res. 109 (E8): E8. doi:10.1029/2004JE002235. Bibcode: 2004JGRE..109.8001M. https://hal.archives-ouvertes.fr/hal-00380066/file/2004JE002235.pdf.
- Feldman, W (2002). "Global distribution of neutrons from Mars: Results from Mars Odyssey". Science 297 (5578): 75–78. doi:10.1126/science.1073541. PMID 12040088. Bibcode: 2002Sci...297...75F.
- Feldman, W. (2008). "North to south asymmetries in the water-equivalent hydrogen distribution at high latitudes on Mars". J. Geophys. Res. 113 (E8). doi:10.1029/2007JE003020. Bibcode: 2008JGRE..113.8006F.
- "Confirmation of Water on Mars". Nasa.gov. 2008-06-20. http://www.nasa.gov/mission_pages/phoenix/news/phoenix-20080620.html.
- Mutch, T.A. (1976). "The surface of Mars: The view from the Viking2 lander". Science 194 (4271): 1277–1283. doi:10.1126/science.194.4271.1277. PMID 17797083. Bibcode: 1976Sci...194.1277M.
- Mutch, T. (1977). "The geology of the Viking Lander 2 site". J. Geophys. Res. 82 (28): 4452–4467. doi:10.1029/js082i028p04452. Bibcode: 1977JGR....82.4452M.
- Levy, J. (2009). "Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations". J. Geophys. Res. 114 (E1): E01007. doi:10.1029/2008JE003273. Bibcode: 2009JGRE..114.1007L.
- Washburn, A. 1973. Periglacial Processes and Environments. St. Martin’s Press, New York, pp. 1–2, 100–147.
- Mellon, M (1997). "Small-scale polygonal features on Mars: Seasonal thermal contraction cracks in permafrost". J. Geophys. Res. 102 (E11): 25617–25628. doi:10.1029/97je02582. Bibcode: 1997JGR...10225617M.
- Mangold, N (2005). "High latitude patterned grounds on Mars: Classification, distribution and climatic control". Icarus 174 (2): 336–359. doi:10.1016/j.icarus.2004.07.030. Bibcode: 2005Icar..174..336M.
- Marchant, D.; Head, J. (2007). "Antarctic dry valleys: Microclimate zonation, variable geomorphic processes, and implications for assessing climate change on Mars". Icarus 192 (1): 187–222. doi:10.1016/j.icarus.2007.06.018. Bibcode: 2007Icar..192..187M.
- Refubium – Suche
- Kostama, V.-P.; Kreslavsky, Head (2006). "Recent high-latitude icy mantle in the northern plains of Mars: Characteristics and ages of emplacement". Geophys. Res. Lett. 33 (11): L11201. doi:10.1029/2006GL025946. Bibcode: 2006GeoRL..3311201K.
- Malin, M.; Edgett, K. (2001). "Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission". J. Geophys. Res. 106 (E10): 23429–23540. doi:10.1029/2000je001455. Bibcode: 2001JGR...10623429M.
- Milliken, R. (2003). "Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images". J. Geophys. Res. 108 (E6): E6. doi:10.1029/2002JE002005. Bibcode: 2003JGRE..108.5057M.
- Kreslavsky, M.; Head, J. (2000). "Kilometer-scale roughness on Mars: Results from MOLA data analysis". J. Geophys. Res. 105 (E11): 26695–26712. doi:10.1029/2000je001259. Bibcode: 2000JGR...10526695K.
- Seibert, N.; Kargel, J. (2001). "Small-scale martian polygonal terrain: Implications for liquid surface water". Geophys. Res. Lett. 28 (5): 899–902. doi:10.1029/2000gl012093. Bibcode: 2001GeoRL..28..899S.
- Kreslavsky, M.A., Head, J.W., 2002. High-latitude Recent Surface Mantle on Mars: New Results from MOLA and MOC. European Geophysical Society XXVII, Nice.
- Head, J.W.; Mustard, J.F.; Kreslavsky, M.A.; Milliken, R.E.; Marchant, D.R. (2003). "Recent ice ages on Mars". Nature 426 (6968): 797–802. doi:10.1038/nature02114. PMID 14685228. Bibcode: 2003Natur.426..797H.
- Lefort, A.; Russell, P. S.; Thomas, N.; McEwen, A. S.; Dundas, C. M.; Kirk, R. L. (2009). "Observations of periglacial landforms in Utopia Planitia with the High Resolution Imaging Science Experiment (HiRISE)". Journal of Geophysical Research 114 (E4): E04005. doi:10.1029/2008JE003264. Bibcode: 2009JGRE..114.4005L. https://boris.unibe.ch/36929/.
- Morgenstern, A; Hauber, E; Reiss, D; van Gasselt, S; Grosse, G; Schirrmeister, L (2007). "Deposition and degradation of a volatile-rich layer in Utopia Planitia, and implications for climate history on Mars". Journal of Geophysical Research: Planets 112 (E6): E06010. doi:10.1029/2006JE002869. Bibcode: 2007JGRE..11206010M.
- Lefort, A.; Russell, P.S.; Thomas, N. (2010). "Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE". Icarus 205 (1): 259. doi:10.1016/j.icarus.2009.06.005. Bibcode: 2010Icar..205..259L.
- Zanetti, M.; Hiesinger, H.; Reiss, D.; Hauber, E.; Neukum, G. (2009). "Scalloped Depression Development on Malea Planum and the Southern Wall of the Hellas Basin, Mars". Lunar and Planetary Science 40: p. 2178, abstract 2178. Bibcode: 2009LPI....40.2178Z. http://www.lpi.usra.edu/meetings/lpsc2009/pdf/2178.pdf.
- Huge Underground Ice Deposit on Mars Is Bigger Than New Mexico | Space
- Staff (November 22, 2016). "Scalloped Terrain Led to Finding of Buried Ice on Mars". NASA. http://photojournal.jpl.nasa.gov/catalog/PIA21136.
- "Lake of frozen water the size of New Mexico found on Mars – NASA". November 22, 2016. https://www.theregister.co.uk/2016/11/22/nasa_finds_ice_under_martian_surface/.
- Bramson, A, et al. 2015. Widespread excess ice in Arcadia Planitia, Mars. Geophysical Research Letters: 42, 6566–6574
- "Widespread, Thick Water Ice found in Utopia Planitia, Mars". https://planetarycassie.com/2016/11/04/widespread-thick-water-ice-found-in-utopia-planitia-mars/.
- Stuurman, C., et al. 2016. SHARAD detection and characterization of subsurface water ice deposits in Utopia Planitia, Mars. Geophysical Research Letters: 43, 9484_9491.
- Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
- Bleacher, J. and S. Sakimoto. Pedestal Craters, A Tool For Interpreting Geological Histories and Estimating Erosion Rates. LPSC
- "Feature Image: Pedestal Craters in Utopia". http://themis.asu.edu/feature_utopiacraters.
- McCauley, J. F. (1973). "Mariner 9 evidence for wind erosion in the equatorial and mid-latitude regions of Mars". Journal of Geophysical Research 78 (20): 4123–4137. doi:10.1029/JB078i020p04123. Bibcode: 1973JGR....78.4123M.
- Levy, J. et al. 2008. Origin and arrangement of boulders on the martian northern plains: Assessment of emplacement and modification environments> In 39th Lunar and Planetary Science Conference, Abstract #1172. League City, TX
- Levy, J.; Head, J.; Marchant, D. (2009). "Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial mantle processes". Icarus 202 (2): 462–476. doi:10.1016/j.icarus.2009.02.018. Bibcode: 2009Icar..202..462L.
- S. Fagents, A., P. Lanagan, R. Greeley. 2002. Rootless cones on Mars: a consequence of lava-ground ice interaction. Geological Society, Londo. Special Publications: 202, 295–317.
- PSR Discoveries: Rootless cones on Mars
- Jaeger, W., L. Keszthelyi, A. McEwen, C. Dundas, P. Russell, and the HiRISE team. 2007. EARLY HiRISE OBSERVATIONS OF RING/MOUND LANDFORMS IN ATHABASCA VALLES, MARS. Lunar and Planetary Science XXXVIII 1955.pdf.
- Head, J., J. Mustard. 2006. Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary, Meteorit. Planet Science: 41, 1675–1690.
- Mangold (2007). "Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust". J. Geophys. Res. 112 (E8): E08S04. doi:10.1029/2006JE002835. Bibcode: 2007JGRE..112.8S04M. https://hal.archives-ouvertes.fr/hal-00376813.
- Mustard et al., 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 1. Ancient impact melt in the Isidis Basin and implications for the transition from the Noachian to Hesperian, J. Geophys. Res., 112.
- Mustard (2009). "Composition, Morphology, and Stratigraphy of Noachian Crust around the Isidis Basin". J. Geophys. Res. 114 (7): E00D12. doi:10.1029/2009JE003349. Bibcode: 2009JGRE..114.0D12M.
- Levy, J., et al. 2017. Candidate volcanic and impact-induced ice depressions on Mars. Icarus: 285, 185–194.
- University of Texas at Austin. "A funnel on Mars could be a place to look for life." ScienceDaily. ScienceDaily, 10 November 2016. <www.sciencedaily.com/releases/2016/11/161110125408.htm>.
- Gas jets spawn dark 'spiders' and spots on Mars icecap | Mars Odyssey Mission THEMIS
- Benson, M. 2012. Planetfall: New Solar System Visions
- Spiders Invade Mars – Astrobiology Magazine
- Kieffer H, Christensen P, Titus T. 2006 Aug 17. CO
2 jets formed by sublimation beneath translucent slab ice in Mars' seasonal south polar ice cap. Nature: 442(7104):793-6.
- Kieffer, H. H. (2000). Mars Polar Science 2000 – Annual Punctuated CO2 Slab-ice and Jets on Mars.. http://www.lpi.usra.edu/meetings/polar2000/pdf/4095.pdf. Retrieved 6 September 2009.
- Kieffer, Hugh H. (2003). Third Mars Polar Science Conference (2003)- Behavior of Solid CO. http://www.lpi.usra.edu/meetings/polar2003/pdf/8083.pdf. Retrieved 6 September 2009.
- Portyankina, G., ed (2006). Fourth Mars Polar Science Conference – Simulations of Geyser-Type Eruptions in Cryptic Region of Martian South. http://www.lpi.usra.edu/meetings/polar2006/pdf/8040.pdf. Retrieved 11 August 2009.
- Sz. Bérczi, ed (2004). Lunar and Planetary Science XXXV (2004) – Stratigraphy of Special Layers – Transient Ones on Permeable Ones: Examples. http://www.lpi.usra.edu/meetings/lpsc2004/pdf/1317.pdf. Retrieved 12 August 2009.
- "NASA Findings Suggest Jets Bursting From Martian Ice Cap". Jet Propulsion Laboratory (NASA). 16 August 2006. http://www.jpl.nasa.gov/news/news.cfm?release=2006-100.
- C.J. Hansen; N. Thomas; G. Portyankina; A. McEwen; T. Becker; S. Byrne; K. Herkenhoff; H. Kieffer et al. (2010). "HiRISE observations of gas sublimation-driven activity in Mars' southern polar regions: I. Erosion of the surface". Icarus 205 (1): 283–295. doi:10.1016/j.icarus.2009.07.021. Bibcode: 2010Icar..205..283H. http://www.lpl.arizona.edu/~shane/publications/hansen_etal_icarus_2010.pdf. Retrieved 26 July 2010.
- Lorenz, R. 2014. The Dune Whisperers. The Planetary Report: 34, 1, 8–14
- Lorenz, R., J. Zimbelman. 2014. Dune Worlds: How Windblown Sand Shapes Planetary Landscapes. Springer Praxis Books / Geophysical Sciences.
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
Original source: https://en.wikipedia.org/wiki/Common surface features of Mars. Read more