HiWish program

HiWish is a program created by NASA so that anyone can suggest a place for the HiRISE camera on the Mars Reconnaissance Orbiter to photograph.^[1] It was started in January 2010. In the first few months of the program 3000 people signed up to use HiRISE.^[2][3] The first images were released in April 2010.^[4] Over 7000 suggestions were made by the public; suggestions were made for targets in each of the 30 quadrangles of Mars. Selected images released were used for three talks at the 16th Annual International Mars Society Convention. Below are some of the over 4,224 images that have been released from the HiWish program as of March, 2016.^[5]

Glacial features

Some landscapes look just like glaciers moving out of mountain valleys on Earth. Some have a hollowed-out appearance, looking like a glacier after almost all the ice has disappeared. What is left are the moraines—the dirt and debris carried by the glacier. The center is hollowed out because the ice is mostly gone.^[6] These supposed alpine glaciers have been called glacier-like forms (GLF) or glacier-like flows (GLF).^[7] Glacier-like forms are a later and maybe more accurate term because we cannot be sure the structure is currently moving.^[8]

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Martian glacier moving down a valley, as seen by HiRISE under HiWish program.

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  Possible glacier flowing down a valley and spreading out on a plain. Rectangle shows a portion that is enlarged in the next image.

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  Enlargement of the area in the rectangle in the previous image. This area would be called a moraine in an alpine glacier on Earth.

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  Well-developed hollows of concentric crater fill, as seen by HiRISE under the HiWish program.

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  Glacier on a crater floor, as seen by HiRISE under HiWish program The cracks in the glacier may be crevasses. There is also a gully system on the crater wall.

Ancient rivers and streams

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.^[9] Some are visible in the pictures below.

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  Channel on floor of Newton Crater, as seen by HiRISE under HiWish program.

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  Branched channel, as seen by HiRISE under HiWish program.

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  Branched channel, as seen by HiRISE under HiWish program.

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  Oxbow lake, as seen by HiRISE under HiWish program.

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  Valleys as seen by HiRISE under HiWish program

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  Channel in Arabia, as seen by HiRISE under HiWish program.

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  Channel system that travels through part of a crater, as seen by HiRISE under HiWish program

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  Channels, as seen by HiRISE under HiWish program. Stream appears to have eroded through a hill.

New Crater

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  HiRISE images showing discovery of a new crater with HiWish program

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  New crater, as seen by HiRISE under HiWish program. The new crater indicated with the white arrow is about 10 yards across and was probably created by the collision with an object the size of a large watermelon. This crater did not appear in earlier images of the same region.

Sand dunes

Many locations on Mars have sand dunes. 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 CO2 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.

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  Dunes in two craters, as seen by HiRISE under the HiWish program.

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  Dunes among craters, as seen by HiRISE under HiWish program. Some of these are barchans.

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  Dunes on a crater floor, as seen by HiRISE under HiWish program. Most of these are barchans. Box shows location of next image.

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  Dunes on a crater floor, as seen by HiRISE under HiWish program. Most of these are barchans. Note: this is an enlargement of the center of the previous image.

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  Dunes, as seen by HiRISE under HiWish program. Location is Eridania quadrangle.

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  Defrosting dunes and ice in troughs of polygons, as seen by HiRISE under HiWish program

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  Color view of defrosting dunes and ice in troughs of polygons, as seen by HiRISE under HiWish program

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  Defrosting surface, as seen by HiRISE under HiWish program Frost is disappearing in patches from a dune. The trough boundaries around the polygon shapes still contain frost; hence they are white. Note: the north side (side near top) has not defrosted because the sun is coming from the other side.

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  Wide view of dunes in Moreux Crater, as seen by HiRISE under HiWish program

Landing site

Some of the targets suggested became possible sites for a Rover Mission in 2020. The targets were in Firsoff (crater) and Holden Crater. These locations were picked as two of 26 locations considered for a mission that will look for signs of life and gather samples for a later return to Earth.^[10][11][12]

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  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).

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  Close-up of layers in Firsoff Crater, as seen by HiRISE Note: this is an enlargement of the previous image of Firsoff Crater.

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  Layers in Firsoff crater with a box showing the size of a football field Picture taken by HiRISE under HiWish program.

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  Layers and faults in Firsoff Crater, as seen by HiRISE under HiWish program. Arrows show one large fault, but there are other smaller ones in the picture.

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  Part of delta in Holden Crater, as seen by HiRISE under HiWish program Holden crater is a possible landing site for a Mars Rover scheduled for 2020.^[1]

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  Close view of previous image showing layers, as seen by HiRISE under HiWish program and enlarged with HiView

1. ^ Golombek, J. et al. 2016. Downselection of landing Sites for the Mars 2020 Rover Mission. 47th Lunar and Planetary Science Conference (2016). 2324.pdf

Landscape features

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  Troughs to the East of Albor Tholus, as seen by HiRISE under the HiWish program.

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  Portion of a trough (Fossae) in Elysium Planitia, as seen by HiRISE under the HiWish program. Blue indicates possible seasonal frost.

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  Landslide in a crater, as seen by HiRISE under HiWish program Image from Iapygia quadrangle.

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  Wide view of Buttes and Mesas, as seen by HiRISE under HiWish program Location is Elysium quadrangle.

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  Buttes and mesas, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image.

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  Mesas, as seen by HiRISE under HiWish program Note: this is an enlargement of a previous image.

Dark slope streaks

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  Layers and dark slope streaks, as seen by HiRISE under HiWish program

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  Dark slope streaks on mesa, as seen by HiRISE under HiWish program Location is Amazonis quadrangle.

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  Close-up of some layers under cap rock of a pedestal crater and a dark slope streak, as seen by HiRISE under HiWish program.

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  Dark slope streaks and layers near a pedestal crater, as seen by HiRISE under the HiWish program. Arrows show the small starting points for the streaks.

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  Dark slope streaks on mound in Lycus Sulci in Diacria quadrangle, as seen by HiRISE under HiWish program

Layers

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.^[13] Layers can be hardened by the action of groundwater.

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  Layers exposed at the base of a group of buttes in Mangala Valles in Memnonia quadrangle, as seen by HiRISE under HiWish program. Arrows point to boulders sitting in pits. The pits may have formed by winds, heat from the boulders melting ground ice, or some other process.

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  Buttes, as seen by HiRISE under HiWish program. Buttes have layered rocks with a hard resistant cap rock on the top which protects the underlying rocks from erosion.

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  Butte in Crommelin Crater, as seen by HiRISE under HiWish program. Location is Oxia Palus quadrangle.

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  Layers in Crommelin Crater, as seen by HiRISE under HiWish program. Location is Oxia Palus quadrangle.

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  Light toned butte, as seen by HiRISE, under HiWish program. Light toned material is probably sulfate-rich and similar to material examined by Spirit Rover, and it once probably covered the whole floor.

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  Layered terrain in Aeolis quadrangle, as seen by HiRISE under HiWish program.

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  Layers in Arabia, as seen by HiRISE under HiWish program.

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  Wide view of part of Danielson Crater, as seen by HiRISE under HiWish program

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  Enlargement of previous image of Danielson Crater, as seen by HiRISE under HiWish program The box represents the size of a football field.

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  Close-up of layers in Danielson Crater, as seen by HiRISE under HiWish program—boulders are visible, as well as dark sand

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  Close-up of layers in trough south of Ius Chasma, as seen by HiRISE under HiWish program

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  Close-up of layers in Lotto Crater, as seen by HiRISE under HiWish program

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  Layers, as seen by HiRISE under HiWish program Location is Tempe Terra

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  Layers, as seen by HiRISE under HiWish program Location is Tempe Terra Note: this is an enlargement of the previous image.

Gullies

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.^[14] 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.

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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.

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  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.

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  Gullies on wall of crater, as seen by HiRISE under HiWish program Location is the Mare Acidalium quadrangle.

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  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.

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  Gullies in crater in Phaethontis quadrangle, as seen by HiRISE under HiWish program

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  Gullies along mesa wall in North Tempe Terra, as seen by HiRISE under HiWish program

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  Close view of gully apron, as seen by HiRISE under HiWish program Note this is an enlargement of the previous image.

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  Close view of gully alcove, as seen by HiRISE under HiWish program Note this is an enlargement of a previous image.

Latitude dependent mantle

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.^[15][16][17] In some places a number of layers are visible in the mantle.

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  Surface showing appearance with and without mantle covering, as seen by HiRISE, under the HiWish program. Location is Terra Sirenum in Phaethontis quadrangle.

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  Mantle layers, as seen by HiRISE under HiWish program. Location is Eridania quadrangle

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  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.

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.^{[18][19][20][21][22]} Thermal measurements from orbit suggest ice.^[23][24] The Phoenix (spacecraft) discovered water ice with made direct observations since it landed in a field of polygons.^[25][26] In fact, its landing rockets exposed pure ice. 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.^{[27][28] [29][30][31][32][33]}

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Polygonal patterned ground

Polygonal, patterned ground is quite common in some regions of Mars.^{[34][35][36][37][38][39][40]} 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.^{[15][16][41][42]}

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  High center polygons, shown with arrows, as seen by HiRISE under HiWish program. Loacation is Casius quadrangle. Image enlarged with HiView.

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  Scalloped terrain labeled with both low center polygons and high center polygons, as seen by HiRISE under HiWish program Loacation is Casius quadrangle. Image enlarged with HiView.

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  Low center polygons, as seen by HiRISE under HiWish program Loacation is Casius quadrangle. Image enlarged with HiView.

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  High and low center polygons, as seen by HiRISE under HiWish program Loacation is Casius quadrangle. Image enlarged with HiView.

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  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.

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  Low center polygons, as seen by HiRISE under HiWish program Loacation is Casius quadrangle. Image enlarged with HiView. Location is Casius quadrangle.

Scalloped topography

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^[43][44] in the northern hemisphere and in the region of Peneus and Amphitrites Patera^[45][46] 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.^[47]

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  Scalloped ground, as seen by HiRISE under HiWish program.

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  Close-up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.

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  Scalloped ground, as seen by HiRISE under HiWish program.

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  Close-up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.

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  Low center polygons, shown with arrows, as seen by HiRISE under HiWish program Image was enlarged with HiView.

Ring mold craters

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.

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  Ring mold craters of various sizes on floor of a crater, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.

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  Wide view of a field of ring mold craters, as seen by HiRISE under HiWish program

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  Close view of ring mold crater, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image of a field of ring mold craters.

Halo Craters

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  Pedestal crater with boulders along rim. Such craters are called "halo craters."^[1] Picture taken with HiRISE under HiWish program.

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  Close view of boulders on lower left of crater rim Box is the size of a football field, so boulders are roughly the size of cars or small houses. Picture taken with HiRISE under HiWish program.

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  Close view of boulders along crater rim Boulders are roughly the size of cars or small houses. Picture taken with HiRISE under HiWish program.

1. ^ 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

Dust devil tracks

Dust devil tracks can be very pretty. They are caused by giant dust devils removing bright colored dust from the Martian surface; thereby exposing a dark layer.

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  Dust devil tracks, as seen by HiRISE under HiWish program.

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  Dust devil tracks, as seen by HiRISE under HiWish program

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  Layers in Danielson Crater with dust devil tracks at the top of the picture, as seen by HiRISE under HiWish program

Yardangs

Yardangs are common in some regions on Mars, especially in what's called the "Medusae Fossae Formation." This formation is found in the Amazonis quadrangle and near the equator.^[48] 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.^[49] Because they exhibit very few impact craters they are believed to be relatively young.^[50]

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  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.

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  Yardangs, as seen by HiRISE under HiWish program Location is near Gordii Dorsum in the Amazonis quadrangle. Note: this is an enlargement of previous image.

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  Yardangs, as seen by HiRISE under HiWish program Location is near Gordii Dorsum in the Amazonis quadrangle. Note: this is an enlargement of previous image.

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  Yardangs formed in light-toned material and surrounded by dark, volcanic basalt sand, as seen by HiRISE under HiWish program. Loacation is Margaritifer Sinus quadrangle.

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  Close-up image of yardangs, as seen by HiRISE under HiWish program. Arrows point to transverse aeolian ridges, TAR's, a type of dune. Note this is an enlargement of the previous image from HiRISE.

Upper Plains Unit

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 (Ismenius Lacus quadrangle) region, but it occurs in other places as well. The remnants consist of sets of dipping layers in craters and along mesas.^[51] Sets of dipping layers may be of various sizes and shapes—some look like Aztec pyramids from Central America

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  Layered structure in crater that is probably what is left of a layered unit that once covered a much larger area. Material for this unit fell from the sky as ice-coated dust. The picture was taken by HiRISE, under the HiWish program. Picture is from Hellas quadrangle.

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  Dipping layers, as seen by HiRISE under HiWish program

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  Layered features in crater, as seen by HiRISE under HiWish program

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  Layered structures, as seen by HiRISE under HiWish program

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.

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  Layered features and brain terrain, as seen by HiRISE under HiWish program The upper plains unit often changes into brain terrain.

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  Brain terrain is forming from the breakdown of upper plains unit, as seen by HiRISE under HiWish program Arrow points to a place where fractures are forming that will turn into brain terrain.

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  Brain terrain is forming from the breakdown of upper plains unit, as seen by HiRISE under HiWish program Arrow points to a place where fractures are forming that will turn into brain terrain.

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.

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  Well developed ribbed upper plains material. These start with small cracks that expand as ice sublimates from the surfaces of the crack. Picture was taken with HiRISE under HiWish program

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  Dipping layers, as seen by HiRISE under HiWish program Also, Ribbed Upper plains material is visible in the upper right of the picture. It is forming from the upper plains unit, and in turn is being eroded into brain terrain.

Small cracks often contain small pits and chains of pits; these are thought to be from sublimation (phase transition) of ice in the ground.^[52][53] 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.^[54][55] In a short time, the ice will disappear into the cold, thin atmosphere in a process called sublimation (phase transition). 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.^[25][56] In addition, HiRISE has seen fresh craters with ice at the bottom. After a time, HiRISE saw the ice deposit disappear.^[57]

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.^[53] 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.^[58][59][60]

Linear Ridge Networks

Linear ridge networks are found in various places on Mars in and around craters.^[61] 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.^[62][63][64] Water here could have supported

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  Network of ridges, as seen by HiRISE under HiWish program Ridges may be formed in various ways.

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  Color, close-up of ridges seen in previous image, as seen by HiRISE under HiWish program

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  Close-up and color image of linear ridge network, as seen by HiRISE under HiWish program

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  More linear ridge networks from same location as previous image, as seen by HiRISE under HiWish program

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  Linear ridge networks, as seen by HiRISE under HiWish program Location is Amazonis quadrangle.

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  Linear ridge network, as seen by HiRISE under HiWish program Location is Mare Tyrrhenum quadrangle.

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  Linear ridge network, as seen by HiRISE under HiWish program Location is Casius quadrangle.

Mesas formed by ground collapse

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  Group of mesas, as seen by HiRISE under HiWish program Oval box contains mesas that may have moved apart.

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  Enlarged view of a group of mesas, as seen by HiRISE under HiWish program One surface is forming square shapes.

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  Mesas breaking up forming straight edges, as seen by HiRISE under HiWish program

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  Large group of concentric cracks, as seen by HiRISE, under HiWish program.

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  Tilted layers formed when ground collapsed, as seen by HiRISE, under HiWish program.

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  Tilted layers formed from ground collapse, as seen by HiRISE, under HiWish program.

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  Mesas breaking up into blocks, as seen by HiRISE, under HiWish program.

Fractures forming blocks

In places large fractures break up surfaces. Sometimes straight edges are formed and large cubes are created by the fractures.

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  Wide view of mesas that are forming fractures, as seen by HiRISE under HiWish program.

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  Enlarged view of a part of previous image, as seen by HiRISE under HiWish program. The rectangle represents the size of a football field.

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  Close-up of blocks being formed, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program.

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  Close-up of blocks being formed, as seen by HiRISE under HiWish program The rectangle represents the size of a football field, so blocks are the size of buildings.

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  Close-up of blocks being formed, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program. Many long fractures are visible on the surface.

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  Surface breaking up, as seen by HiRISE under HiWish program as seen by HiRISE under HiWish program. Near the top the surface is eroding into brain terrain.

Lava flows

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  Lava flow in Tharsis quadrangle, as seen by HiRISE under HiWish program

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  Close-up of lava flow with labels, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image of lava flows.

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  Lava flows with older and younger flows labeled, as seen by HiRISE under HiWish program

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  Edge of lava flow, as seen by HiRISE under HiWish program Location is Solis Planum in Phoenicis Lacus quadrangle.

Mud volcanoes

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.

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  Large field of cones that may be mud volcanoes, as seen by HiRISE under HiWish program

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  Close-up of possible mud volcanoes, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image.

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  Possible mud volcano, as seen by HiRISE under HiWish program

How to suggest image

To suggest a location for HiRISE to image visit the site at http://www.uahirise.org/hiwish

In the sign up process you will need to come up with an ID and a password. When you choose a target to be imaged, you have to pick and exact location on a map and write about why the image should be taken. If you suggestion is accepted, it may take 3 months or more to see your image. You will be sent an email telling you about your images. The emails usually arrive on the first Wednesday of the month in the late afternoon.

See also

• Climate of Mars
• Geology of Mars
• Glaciers
• Glaciers on Mars
• Barchan
• Groundwater on Mars
• Martian gullies
• Linear ridge networks
• Yardangs on Mars

References

1. "Public Invited To Pick Pixels On Mars". Mars Daily. January 22, 2010. Retrieved January 10, 2011.
2. Interview with Alfred McEwen on Planetary Radio, 3/15/2010
3. http://www.planetary.org/multimedia/planetary-radio/show/2010/384.html
4. "NASA releases first eight "HiWish" selections of people’s choice Mars images". TopNews. April 2, 2010. Retrieved January 10, 2011.
5. McEwen, A. et al. 2016. THE FIRST DECADE OF HIRISE AT MARS. 47th Lunar and Planetary Science Conference (2016) 1372.pdf
6. Milliken, R., J. Mustard, D. Goldsby. 2003. Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images. J. Geophys. Res. 108. doi:10.1029/2002JE002005.
7. Arfstrom, J and W. Hartmann. 2005. Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships. Icarus 174, 321-335.
8. Hubbard B., R. Milliken, J. Kargel, A. Limaye, C. Souness. 2011. Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars Icarus 211, 330–346
9. Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
10. http://marsnext.jpl.nasa.gov/workshops/index.cfm
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Recommended reading

• 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.

External links

• Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention
• https://www.youtube.com/watch?v=RYG-HLr33CM Martian Geology - Jim Secosky - 16th Annual International Mars Society Convention
• https://www.youtube.com/watch?v=ZNTNzQy1_UA Walks on Mars - Jim Secosky - 16th Annual International Mars Society Convention