Margaritifer Terra

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Margaritifer Terra is an ancient, heavily cratered region of Mars. It is centered just south of the Martian equator at Lua error in package.lua at line 80: module 'strict' not found. and covers 2600 km at its widest extent. The area reveals "chaos terrain", outflow channels, and alluvial plains that are indicative of massive flooding. Wind erosion patterns are also in evidence. A region within the terra shows some of the highest valley network densities on the planet. Ares Vallis is another notable feature, where the flood and flow patterns are in evidence; it was the landing site of Mars 6 and NASA's Mars Pathfinder.[citation needed] It is also one of several proposed landing sites for the Mars 2020 Rover.[1]

Holden and Eberswalde, craters in Margaritifer Terra are thought to have formerly held lakes because they contain deltas and iron/magnesium smectite minerals which need water to form.[2] The * Uzboi-Landon-Morava (ULM) system of paths for water flow is found in Margaritifer Terra.

Margaritifer Terra was named in 1979, after the Pearl Coast, south India. Part of it is found in the Margaritifer Sinus quadrangle and part in the Oxia Palus quadrangle.

  • MOLA map showing boundaries for Margaritifer Terra and other regions. Color indicates elevation.


Layers

Some of the images from this quadrangle display 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.[3] A detailed discussion of layering with many Martian examples can be found in Sedimentary Geology of Mars.[4]

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. <templatestyles src="Module:Hatnote/styles.css"></templatestyles>

Main article: Groundwater on Mars § Layered terrain

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  • Butte in Arsinoes Chaos with some light-toned layers, as seen by HiRISE under HiWish program.

  • Light-toned deposit in Arsinoes Chaos, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Light-toned deposit in Arsinoes Chaos, as seen by HiRISE under HiWish program. Note: this field can be found in the previous wide image of Arsinoes Chaos, as seen by CTX camera (on Mars Reconnaissance Orbiter).

  • Layered butte, as seen by HiRISE under HiWish program.

  • 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.

  • Light toned butte, as seen by HiRISE, under HiWish program.

  • Close up of top of light toned butte, as seen by HiRISE under HiWish program.

  • THEMIS image of wide view of following HiRISE images. Black box shows approximate location of HiRISE images. This image is just a part of the vast area known as Aureum Chaos. Click on image to see more details.

  • Aureum Chaos, as seen by HiRISE, under the HiWish program.

  • Close up view of previous image, as seen by HiRISE under HiWish program. Small round dots are boulders.

  • Huge canyons in Aureum Chaos. Gullies are rare at this latitude. Picture taken by THEMIS.

  • Aureum Chaos, as seen from THEMIS.

On April 1, 2010, NASA released the first images under the HiWish program, with the public suggesting places for HiRISE to photograph. One of the eight locations was Aureum Chaos.[5] The first image below gives a wide view of the area. The next two images are from the HiRISE image.[6]

  • THEMIS image of wide view of following HiRISE images. Black box shows approximate location of HiRISE images. This image is just a part of the vast area known as Aureum Chaos. Click on image to see more details.

  • Aureum Chaos, as seen by HiRISE, under the HiWish program.

  • Close up view of previous image, as seen by HiRISE under HiWish program. Small round dots are boulders.

Yardangs

  • Yardangs formed in light-toned material and surrounded by dark, volcanic basalt sand, as seen by HiRISE under HiWish program.

  • 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.

References

  1. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  2. ↑ Murchie, S. et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114.
  3. ↑ Lua error in package.lua at line 80: module 'strict' not found.
  4. ↑ Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
  5. ↑ Captioned Images Inspired by HiWish Suggestions (HiRISE)
  6. ↑ Mesas in Aureum Chaos (HiRISE image; Observation ID: ESP_016869_1775)

See also

External links

  • [1] Lakes on Mars - Nathalie Cabrol (SETI Talks)


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