Astronomy:Medusae Fossae Formation

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Medusa Fossae
Medusae Fossae based on day THEMIS.png
Medusae Fossae based on THEMIS day-time image
CoordinatesCoordinates: 3°12′S 163°00′W / 3.2°S 163.0°W / -3.2; -163.0
Length333.0 km

The Medusae Fossae Formation is a large geological unit of probable volcanic origin on the planet Mars.[1] It is named for the Medusa of Greek mythology. "Fossae" is Latin for "trenches". Located roughly at 5°S 213°E / 5°S 213°E / -5; 213, 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 (discontinuously) for more than 5,000 km along the equator of Mars. It has an area equal to 20% the size of the continental United States.[2] 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.[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] Comparisons of elemental composition suggest that the Medusae Fossae Formation has been the main source of Mars' ubiquitous surface dust.[2] In July 2018, researchers reported that, indeed, the largest single source of dust on the planet Mars is the Medusae Fossae Formation.[2]

An analysis of data from the Mars Odyssey Neutron Spectrometer revealed that the western lobe of the Medusae Fossae Formation contains water. This means that this formation contains bulk water ice. During periods of high obliquity (tilt) water ice was stable on the surface.[8]

Combining several gravity models of Mars with the MOLA topographic dataset allowed calculation of the density of the deposit; the value is 1.765 ± 0.105 g/cm3, similar to the density of terrestrial ignimbrites.[9] This rules out significant amounts of ice in the bulk composition. In combination with the deposit's high content of sulfur and chlorine, it implies an explosive volcanic origin. The total volume of the deposit is 1.4 × 106 km3; such a large deposit might have been emplaced in periodic eruptions over an interval of 500 million years.[9]

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.[10]


The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs.[11] 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.[12] Layers are seen in parts of the formation. A resistant caprock on the top of yardangs has been observed in Viking,[13] Mars Global Surveyor,[14] and HiRISE photos.[15] 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.[16]

See also


  1. 1.0 1.1 "The Medusa Fossae formation on Mars". European Space Agency. 29 March 2005. 
  2. 2.0 2.1 2.2 Ojha, Lujendra; Lewis, Kevin; Karunatillake, Suniti; Schmidt, Mariek (2018). "The Medusae Fossae Formation as the single largest source of dust on Mars". Nature Communications 9 (1): 2867. doi:10.1038/s41467-018-05291-5. PMID 30030425. Bibcode2018NatCo...9.2867O. 
  3. Watters, T. R.; Campbell, B.; Carter, L.; Leuschen, C. J.; Plaut, J. J.; Picardi, G.; Orosei, R.; Safaeinili, A. et al. (2007). "Radar Sounding of the Medusae Fossae Formation Mars: Equatorial Ice or Dry, Low-Density Deposits?". Science 318 (5853): 1125–1128. doi:10.1126/science.1148112. PMID 17975034. Bibcode2007Sci...318.1125W. 
  4. Orosei, R.; Cantini, F.; Caprarelli, G.; Carter, L. M.; Papiano, I.; Rossi, A. P. (2016). "Radar Sounding by MARSIS over Lucus Planum, Mars". Lunar and Planetary Science Conference (1903): 1869. Bibcode2016LPI....47.1869O. 
  5. Kerber, Laura; Head, James W.; Madeleine, Jean-Baptiste; Forget, François; Wilson, Lionel (2012). "The dispersal of pyroclasts from ancient explosive volcanoes on Mars: Implications for the friable layered deposits". Icarus 219 (1): 358–381. doi:10.1016/j.icarus.2012.03.016. Bibcode2012Icar..219..358K. 
  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. 
  7. Greeley, Ronald; Guest, J.E. (1987). Geologic map of the eastern equatorial region of Mars. doi:10.3133/i1802B. 
  8. Wilson, Jack T.; Eke, Vincent R.; Massey, Richard J.; Elphic, Richard C.; Feldman, William C.; Maurice, Sylvestre; Teodoro, Luís F.A. (2018). "Equatorial locations of water on Mars: Improved resolution maps based on Mars Odyssey Neutron Spectrometer data". Icarus 299: 148–160. doi:10.1016/j.icarus.2017.07.028. Bibcode2018Icar..299..148W. 
  9. 9.0 9.1 Ojha, Lujendra; Lewis, Kevin (2018). "The Density of the Medusae Fossae Formation: Implications for its Composition, Origin, and Importance in Martian History". Journal of Geophysical Research: Planets 123 (6): 1368–1379. doi:10.1029/2018JE005565. Bibcode2018JGRE..123.1368O. 
  10. Zimbelman, James R.; Griffin, Lora J. (2010). "HiRISE images of yardangs and sinuous ridges in the lower member of the Medusae Fossae Formation, Mars". Icarus 205 (1): 198–210. doi:10.1016/j.icarus.2009.04.003. Bibcode2010Icar..205..198Z. 
  11. Bridges, Nathan T.; Muhs, Daniel R. (2012). "Duststones on Mars: Source, Transport, Deposition, and Erosion". Sedimentary Geology of Mars. pp. 169–182. doi:10.2110/pec.12.102.0169. ISBN 978-1-56576-312-8. 
  13. Scott, David H.; Tanaka, Kenneth L. (1982). "Ignimbrites of Amazonis Planitia Region of Mars". Journal of Geophysical Research: Solid Earth 87: 1179–1190. doi:10.1029/JB087iB02p01179. Bibcode1982JGR....87.1179S. 
  14. Malin, M. C.; Carr, M. H.; Danielson, G. E.; Davies, M. E.; Hartmann, W. K.; Ingersoll, A. P.; James, P. B.; Masursky, H. et al. (1998). "Early Views of the Martian Surface from the Mars Orbiter Camera of Mars Global Surveyor". Science 279 (5357): 1681–1685. doi:10.1126/science.279.5357.1681. PMID 9497280. Bibcode1998Sci...279.1681M. 
  15. Mandt, Kathleen E.; De Silva, Shanaka L.; Zimbelman, James R.; Crown, David A. (2008). "Origin of the Medusae Fossae Formation, Mars: Insights from a synoptic approach". Journal of Geophysical Research 113 (E12): E12011. doi:10.1029/2008JE003076. Bibcode2008JGRE..11312011M.