Medusae Fossae Formation

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Medusa Fossae
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Medusae Fossae based on THEMIS day-time image
Coordinates Lua error in Module:Coordinates at line 668: callParserFunction: function "#coordinates" was not found.
Length 333.0 km

The Medusae Fossae Formation is a large geological unit of uncertain origin on the planet Mars.[1] It is named for the Medusa of Greek mythology. "Fossae" is Latin for "trenches". Located roughly at Lua error in Module:Coordinates at line 668: callParserFunction: function "#coordinates" was not found., it straddles the highland - lowland boundary near the Tharsis and Elysium volcanic areas. The Medusae Fossae Formation lies partly in five quadrangles: the Amazonis quadrangle, the Tharsis quadrangle, the Memnonia quadrangle, the Elysium quadrangle, and the Aeolis quadrangle.

The Medusae Fossae Formation is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars. Sometimes, the formation appears as a smooth and gently undulating surface, however in places it is wind-sculpted into ridges and grooves.[1] Radar imaging has suggested that the region may contain either extremely porous rock (for example volcanic ash) or deep layers of glacier-like ice deposits amounting to about the same quantity as is stored in Mars' south polar cap.[2][3][4] Using a global climate model, a group of researchers headed by Laura Kerber found that the Medusae Fossae Formation could have been formed from ash from the volcanoes Apollinaris Mons, Arsia Mons, and possibly Pavonis Mons.[5] Further evidence for a fine-grained composition is the fact that the area gives almost no radar return. For this reason it has been called a "stealth" region.[6] The formation is divided into three subunits (members) that are all considered to be of Amazonian age, the youngest era in martian geological history.[7]

Inverted relief

The lower portion (member) of Medusae Fossae Formation contains many patterns and shapes that are thought to be the remains of streams. It is believed that streams formed valleys that were filled and became resistant to erosion by cementation of minerals or by the gathering of a coarse covering layer to form an inverted relief. These inverted stream beds are sometimes called sinuous ridges or raised curvilinear features. They have been divided into six classes: flat-crested, narrow-crested, round-crested, branching, non-branching, and multilevel. They may be a kilometer or so in length. Their height ranges from a meter to greater than 10 meters, while the width of the narrow ones is less than 10 meters.[8][9]

Yardangs

The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs.[10] These ridges generally point in direction of the prevailing winds that carved them, and demonstrate the erosive power of martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles, and was most likely formed by the deposition of wind-blown dust or volcanic ash. Yardangs are parts of rock that have been sand blasted into long, skinny ridges by bouncing sand particles blowing in the wind.[11] Layers are seen in parts of the formation. A resistant caprock on the top of yardangs has been observed in Viking,[12] Mars Global Surveyor,[13] and HiRISE photos.[14] Images from spacecraft show that they have different degrees of hardness probably because of significant variations in the physical properties, composition, particle size, and/or cementation. Very few impact craters are visible throughout the area so the surface is relatively young.[15]

See also

References

  1. 1.0 1.1 "The Medusa Fossae formation on Mars". European Space Agency. 29 March 2005.<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  2. Shiga, David (1 November 2007). "Vast amount of water ice may lie on Martian equator". New Scientist Space. Retrieved 20 January 2011.<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  3. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  4. Orosei, R. et al. 2016. RADAR SOUNDING BY MARSIS OVER LUCUS PLANUM, MARS. 47th Lunar and Planetary Science Conference (2016) 1869.pdf.
  5. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  6. Barlow, Nadine G. (2008). Mars: an introduction to its interior, surface and atmosphere. Cambridge, UK: Cambridge University Press. pp. 75–76. ISBN 978-0-521-85226-5.<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  7. Scott, D.; Tanaka, K. (1986). "Geologic map of the western equatorial region of Mars" (PDF). U.S. Geol. Survey Misc. Invest Series Map 1:15,000,000.<templatestyles src="Module:Citation/CS1/styles.css"></templatestyles>
  8. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  9. http://www.sciencedirect.com/science/journal/00191035
  10. Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
  11. http://www.uahirise.org/ESP_039563_1730
  12. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  13. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  14. Lua error in Module:Citation/CS1/Identifiers at line 47: attempt to index field 'wikibase' (a nil value).
  15. http://themis.asu.edu/zoom-20020416a