Margaritifer Terra is an ancient, heavily cratered region of Mars. It is centered just south of the Martian equator at Coordinates:  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. It is also one of several proposed landing sites for the Mars 2020 Rover.
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. The * Uzboi-Landon-Morava (ULM) system of paths for water flow is found in Margaritifer Terra.
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. 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.
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.
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.
Huge canyons in Aureum Chaos. Gullies are rare at this latitude. Picture taken by 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. The first image below gives a wide view of the area. The next two images are from the HiRISE image.
- Blue, Jennifer. "Margaritifer Terra". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
- "Choosing a place to land NASA's next Mars rover". Arizona State University News. 16 May 2014. Retrieved 2014-05-17.
- 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.
- "HiRISE | High Resolution Imaging Science Experiment". Hirise.lpl.arizona.edu?psp_008437_1750. Retrieved 2012-08-04.
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
- Captioned Images Inspired by HiWish Suggestions (HiRISE)
- Mesas in Aureum Chaos (HiRISE image; Observation ID: ESP_016869_1775)
- Areas of chaos terrain on Mars
- Geography of Mars
- Groundwater on Mars
- Lakes on Mars
- Uzboi-Landon-Morava (ULM)
- J.A. Grant, 'Valley Evolution in Margaritifer Sinus, Mars'
- Geologic Map of MTM -15027, -20027, -25027, and -25032 Quadrangles, Margaritifer Terra Region of Mars United States Geological Survey
-  Lakes on Mars - Nathalie Cabrol (SETI Talks)
|This article about the planet Mars or its moons is a stub. You can help Wikipedia by expanding it.|
|This article about an extraterrestrial geological feature is a stub. You can help Wikipedia by expanding it.|