Margaritifer Terra

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

Margaritifer Terra (/ˌmɑːrɡəˈrɪtəfər ˈtɛrə/) is an ancient, heavily cratered region of Mars. It is centered just south of the Martian equator at 4°54′S 25°00′W / 4.9°S 25°W / -4.9; -25 and covers 2600 km at its widest extent.[1] 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 the Soviet Mars 6 lander[2] and NASA's Mars Pathfinder.[3] It is also one of several proposed landing sites for the Mars 2020 Rover.[4]

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.[5] The Uzboi-Landon-Morava (ULM) system of paths for water flow is found in Margaritifer Terra. Researchers think that great flood channels in this region were carved quickly in just weeks or months by catastrophic outflows of groundwater.[6] Because forming hematite requires liquid water, which could not long exist without a thick atmosphere, Mars must have had a much thicker atmosphere at some time in the past.[7]

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.

  1. ^ "Margaritifer Terra". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  2. ^ "Mars 6". US National Space Science Data Centre. Retrieved 12 April 2013.
  3. ^ "Mars Pathfinder Science Results". NASA. Archived from the original on 2008-09-20. Retrieved 2008-06-09.
  4. ^ "Choosing a place to land NASA's next Mars rover". Arizona State University News. 16 May 2014. Retrieved 2014-05-17.
  5. ^ 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.
  6. ^ "HiRISE | Uplifted Blocks of Light-Toned Layered Deposits (ESP_054753_1825)".
  7. ^ "Mars Odyssey Mission THEMIS: Discoveries". themis.asu.edu. Archived from the original on 2006-01-01.