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HiWish program

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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. The first images were released in April 2010.[2] Over 5000 suggestions were made by the public. Below are some of the over 1100 images that have been released from the HiWish program as of March 2015.

Glacial features

Some landscapes look just like glaciers moving out of mountain valleys on Earth. Some have a hallowed 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.[3] These supposed alpine glaciers have been called glacier-like forms (GLF) or glacier-like flows (GLF). [4] Glacier-like forms are a later and maybe more accurate term because we cannot be sure the structure is currently moving. [5]

Main article: Glaciers on Mars

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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.
    Possible glacier flowing down a valley and spreading out on a plain. Rectangle shows a portion that is enlarged in the next image.
  • Enlargement of the area in the rectangle in the previous image. This area would be called a moraine in an alpine glacier on Earth.
    Enlargement of the area in the rectangle in the previous image. This area would be called a moraine in an alpine glacier on Earth.
  • Well-developed hollows of concentric crater fill, as seen by HiRISE under the HiWish program.
    Well-developed hollows of concentric crater fill, as seen by HiRISE under the HiWish program.

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.

  • Dunes in two craters, as seen by HiRISE under the HiWish program.
    Dunes in two craters, as seen by HiRISE under the HiWish program.
  • Dunes among craters, as seen by HiRISE under HiWish program. Some of these are barchans.
    Dunes among craters, as seen by HiRISE under HiWish program. Some of these are barchans.
  • Dunes on a crater floor, as seen by HiRISE under HiWish program. Most of these are barchans. Box shows location of next image.
    Dunes on a crater floor, as seen by HiRISE under HiWish program. Most of these are barchans. Box shows location of next image.
  • 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.
    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.

Landscape features

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

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

Main article: Groundwater on Mars § Layered terrain

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

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.[7] 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.

Main article: Martian gullies

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

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[8][9] in the northern hemisphere and in the region of Peneus and Amphitrites Patera[10][11] 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.[12]


  • Scalloped ground, as seen by HiRISE under HiWish program.
    Scalloped ground, as seen by HiRISE under HiWish program.
  • 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.
    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.
  • Scalloped ground, as seen by HiRISE under HiWish program.
    Scalloped ground, as seen by HiRISE under HiWish program.
  • 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.
    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.

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.

Main article: Ring mold crater

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


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

References

  1. ^ "Public Invited To Pick Pixels On Mars". Mars Daily. January 22, 2010. Retrieved January 10, 2011.
  2. ^ "NASA releases first eight "HiWish" selections of people's choice Mars images". TopNews. April 2, 2010. Retrieved January 10, 2011.
  3. ^ 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.
  4. ^ Arfstrom, J and W. Hartmann. 2005. Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships. Icarus 174, 321-335.
  5. ^ 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
  6. ^ "HiRISE | High Resolution Imaging Science Experiment". Hirise.lpl.arizona.edu?psp_008437_1750. Retrieved 2012-08-04.
  7. ^ Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and surface runoff on Mars. Science 288, 2330–2335.
  8. ^ 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). Bibcode:2009JGRE..11404005L. doi:10.1029/2008JE003264.
  9. ^ 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" (PDF). Journal of Geophysical Research - Planets. 112 (E6): E06010. Bibcode:2007JGRE..11206010M. doi:10.1029/2006JE002869.
  10. ^ 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. Bibcode:2010Icar..205..259L. doi:10.1016/j.icarus.2009.06.005.
  11. ^ 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" (PDF). Lunar and Planetary Science. 40. p. 2178, abstract 2178. Bibcode:2009LPI....40.2178Z.
  12. ^ http://hiroc.lpl.arizona.edu/images/PSP?diafotizo.php?ID=PSP_002296_1215

See also

  • 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.
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