Martian chaos terrain

From Wikipedia, the free encyclopedia
Jump to: navigation, search

Chaos terrain on Mars is distinctive; nothing on Earth compares to it. Chaos terrain generally consists of irregular groups of large blocks, some tens of kilometers across and a hundred or more meters high. The tilted and flat topped blocks form depressions hundreds of metres deep.[1] A chaotic region can be recognized by a rat's nest of mesas, buttes, and hills, chopped through with valleys which in places look almost patterned.[2][3][4] Some parts of this chaotic area have not collapsed completely—they are still formed into large mesas, so they may still contain water ice.[5] Chaos regions formed long ago. By counting craters (more craters in any given area means an older surface) and by studying the valleys' relations with other geological features, scientists have concluded the channels formed 2.0 to 3.8 billion years ago.[6]


The greatest concentrations of chaotic terrain are in the same locations as giant, ancient river valleys. Because so many large channels seem to originate from chaotic terrain, it is widely believed that chaos terrain is caused by water coming out the ground in the form of massive floods.[7][8] Most of the chaotic terrain exists in the highlands of Mars, south of Chryse Planitia, in the Oxia Palus quadrangle, and along the Martian dichotomy. But some chaos regions can be found in Margaritifer Sinus quadrangle, Phaethontis quadrangle, and Lunae Palus quadrangle.

Theories for formation[edit]

Many different theories have been advanced for how floods of water came to be released with the formation of chaotic terrain. Evidence for the involvement of water has been found—minerals associated with water, such as grey, crystalline hematite and phyllosilicates, are present in chaos regions.[9] Many explanations for the creation of chaos involve the sudden melting of giant reservoirs of ground ice. Some researchers have suggested that a frozen layer, called a cryosphere, developed over a long time period and then something triggered it to rupture and melt suddenly. The rupturing event may have been impacts,[10] magma movements,[11][12] seismic activity,[13] volcanic tectonic strains,[14] increased pore pressure, or the dissociation of clathrates.[15][16][17][18] A clathrate composed of carbon dioxide and methane could have explosively dissociated, thereby liquefying water-saturated sediments. A variation of this idea of a cryosphere is that an aquifer was created along with the cryosphere. As more and more ice was added resulting in a thicker cryosphere, the water in the aquifer became pressurized.[19] When something like an impact or movement of magma broke or melted the cryosphere, floods of water under great pressure were released. However, further calculations showed that the great channels could not have been produced with just a single discharge.[20] Later proposals advanced the notion that the geological shapes present in chaos regions could have been made by a series of over a 100 flooding events.[21]

Melting of buried ice[edit]

More recently, researchers have suggested ways for the formation of chaos without the need for a special triggering event. Tanja Zegers and others calculated that the simple burial of ice-rich sediments could result in the release of huge amounts of water leading to the formation of the large river basins that are associated with most chaos terrains. The group studied Aram Chaos, a large region of chaos that probably began as a large impact crater. In their model, ice-rich material accumulated in the crater and then became covered with sediment, which prevented the ice from disappearing into the thin atmosphere. Eventually, the heat from the deep subsurface together with the insulating qualities of the covering layer produced a thick water layer. Since dense materials tend to sink into water, the overlying rock broke under the strain. The dense, rocky cap fractured into various sized, tilted blocks. The melt water went to the top and made a channel which eroded more and more as water rushed outward. Along with water from other chaotic regions, there would have been enough erosive force to carve the large river valleys we now observe.[22] There is ample evidence for buried deposits of ice in the form of glaciers, preserved under a thin covering of rock and dirt.[23]

It also seems that Mars has had many ice ages in which ice was deposited, then later buried. These ice ages are caused by the frequent large changes in the tilt of the planet.[24] The tilt of the spin axis of Mars is highly variable due to the lack of a large moon.[25][26][27] Observations of many craters have shown that many craters are mostly full of sediments—ice could be one of the sediments. Many craters appear to be very shallow, but observations of younger craters have demonstrated that impact craters start out as sort of bowl shaped; hence a crater that today looks shallow has probably been filled with sediments.[28][29] Research, published by Rodriguez and others in 2005, suggested that the subsurface of Mars contains an accumulation of old craters that may be filled with water or ice.[30]

Sublimation of an ice-rich layer[edit]

Some regions of chaos may have been produced by another means. Galaxias Chaos is different from many other chaotic regions. It does not have associated outflow channels, and it does not display a great elevation difference between it and the surrounding land area, as most of the other chaos regions. Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer, called the Vastitas Borealis Formation (VBF).[31] It is generally believed that the VBF is a residue from water-rich materials deposited by large floods.[32][33] The VBF may have been of varied thickness and may have contained varied amounts of ice. In the thin atmosphere of Mars, this layer would have slowly disappeared by sublimation (changing from a solid directly to a gas). Since some areas would have sublimated more than others, the upper lava cap would not be supported evenly and would crack. Cracks/troughs may have begun from sublimation and shrinkage along the edges of the lava cap. Stress from the undermining of the cap edge would have made cracks in the cap. Places with cracks would undergo more sublimation, then the cracks would widen and form the blocky terrain characteristic of regions of chaos. The sublimation process may have been aided by heat (geothermal flux) from magma movements. There are volcanoes, namely Elysium Montes and Hecates Tholus, nearby which most likely are surrounded by dikes, which would have heated the ground. Also, a warmer period in the past would have increased the amount of water sublimating from the ground.[10]


Chaos terrain seems to be strong evidence for large amounts of water flowing on Mars in the past. Some of the terrain is not totally broken up, so perhaps more water exists frozen inside some of the blocks.


Chaos regions in Margaritifer Sinus quadrangle[edit]

Chaos regions in Oxia Palus quadrangle[edit]

Chaos regions in Phaethontis quadrangle[edit]

Chaos regions in Lunae Palus quadrangle[edit]

On April 1, 2010, NASA released the first images under the HiWish program in which just plain folk suggested places for HiRISE to photograph. One of the eight locations was Aureum Chaos.[34] The first image below gives a wide view of the area. The next two images are from the HiRISE image.[35]

See also[edit]


  1. ^ Meresse, S.; et al. (2008). "Formation and evolution of the chaotic terrains by subsidence and magmatism: Hydraotes Chaos, Mars". Icarus. 194 (2): 487–500. Bibcode:2008Icar..194..487M. doi:10.1016/j.icarus.2007.10.023. 
  2. ^ Sharp, R. (1973). "Mars: Fretted and chaotic terrains". J. Geophys. Res. 78 (20): 4073–4083. Bibcode:1973JGR....78.4073S. doi:10.1029/JB078i020p04073. 
  3. ^ Carr, M. 2006. The Surface of Mars. Cambridge University Press. ISBN 978-0-521-87201-0
  4. ^ Forget, F., et al. 2006. Planet Mars Story of Another World. Praxis Publishing, Chichester, UK. ISBN 978-0-387-48925-4
  5. ^
  6. ^
  7. ^ Carr, M. 1978. Formation of martian flood features by release of water from confined aquifers. NASA Technical Memorandum 79729. 260-262.
  8. ^ Carr, M. (1979). "Formation of martian flood features by release of water from confined aquifers". J. Geophys. Res. 84: 2995–3007. Bibcode:1979JGR....84.2995C. doi:10.1029/JB084iB06p02995. 
  9. ^ Glotch, Timothy D. (2005). "Geologic and mineralogic mapping of Aram Chaos: Evidence for a water-rich history". Journal of Geophysical Research. 110. Bibcode:2005JGRE..11009006G. doi:10.1029/2004JE002389. 
  10. ^ a b c Pedersen, G.; Head, J. (2011). "Chaos formation by sublimation of volatile-rich substrate: evidence from Galaxias Chaos, Mars". Icarus. 211: 316–329. Bibcode:2011Icar..211..316P. doi:10.1016/j.icarus.2010.09.005. 
  11. ^ Chapman, M.; Tanaka, K. (2002). "Related magma-ice interactions: Possible origins of Chasma chaos and surface materials in Xanthe, Margaritifer, and Merdiani Terrae, Mars". Icarus. 155 (2): 324–339. Bibcode:2002Icar..155..324C. doi:10.1006/icar.2001.6735. 
  12. ^ Head, J. and L. Wilson. 2002. Mars: A review and synthesis of general environments and geological settings of Magma-H2O interactions. In: SmeilieJ. And M. Chapman. (EDS.). Volcanic-ice Interactions on Earth and Mars. Geological Society. London
  13. ^ Tanaka, K. (1999). "Debris-flow origin for Simud/Tiu deposits on Mars". J. Geophys. Res. 104: 8637–8652. Bibcode:1999JGR...104.8637T. doi:10.1029/98JE02552. 
  14. ^ Cabrol, Nathalie A.; et al. (1997). "A model of outflow generation by hydrothermal underpressure drainage in volcano-tectonic environment. Shalbatana Vallis (Mars)". Icarus. 125 (2): 455–464. Bibcode:1997Icar..125..455C. doi:10.1006/icar.1996.5625. 
  15. ^ Milton, DJ (1974). "Carbon dioxide hydrate and floods on Mars". Science. 183 (4125): 654–656. Bibcode:1974Sci...183..654M. doi:10.1126/science.183.4125.654. PMID 17778840. 
  16. ^ Hoffmann, H. (2000). "White Mars: A new model for Mars' surface and atmosphere based CO2". Icarus. 146 (2): 326–342. Bibcode:2000Icar..146..326H. doi:10.1006/icar.2000.6398. 
  17. ^ Komatsu, G. et al. 2000. A chaotic terrain formation hypothesis: Explosive outgas and outflow by dissociation of clathrate on Mars. Lunar Planet. Sci. XXXI. 1434.
  18. ^ Rodriguez, J. A. P.; Kargel, Jeffrey; Crown, David A.; Bleamaster, Leslie F.; Tanaka, Kenneth L.; Baker, Victor; Miyamoto, Hideaki; Dohm, James M.; Sasaki, Sho; Komatsu, Goro (2006). "Headward growth of chasmata by volatile outbursts, collapse, and drainage: Evidence from Ganges chaos, Mars". Geophysical Research Letters. 33 (18): 18203. Bibcode:2006GeoRL..3318203R. doi:10.1029/2006GL026275. 
  19. ^ Clifford, S. (1993). "A model for the hydrologic and climatic behaviour of water on mars". J. Geophys. Res. 98: 10973–11016. Bibcode:1993JGR....9810973C. doi:10.1029/93JE00225. 
  20. ^ Baker, V. (2001). "Water and the martian landscape". Nature. 412 (6843): 228–236. doi:10.1038/35084172. PMID 11449284. 
  21. ^ Harrison, Keith P.; Grimm, Robert E. (2008). "Multiple flooding events in Martian outflow channels". Journal of Geophysical Research. 113. Bibcode:2008JGRE..11302002H. doi:10.1029/2007je002951. 
  22. ^ a b Zegers, T.; et al. (2010). "Melt and collapse of buried water ice: An alternative hypothesis for the formation of chaotic terrains on Mars". Earth and Planetary Science Letters. 297 (3–4): 496–504. Bibcode:2010E&PSL.297..496Z. doi:10.1016/j.epsl.2010.06.049. 
  23. ^ Head, J.; Neukum, G.; Jaumann, R.; Hiesinger, H.; Hauber, E.; Carr, M.; Masson, P.; Foing, B.; Hoffmann, H.; et al. (2005). "Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars". Nature. 434 (7031): 346–350. Bibcode:2005Natur.434..346H. doi:10.1038/nature03359. PMID 15772652. 
  24. ^ Head, J.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for the late Amazonian obliquity-driven climate change". Earth Planet. Sci. Lett. 241 (3–4): 663–671. Bibcode:2006E&PSL.241..663H. doi:10.1016/j.epsl.2005.11.016. 
  25. ^ Madeleine, J. et al. 2007. Mars: A proposed climatic scenario for northern mid-latitude glaciation. Lunar Planet. Sci. 38. Abstract 1778.
  26. ^ Madeleine, J.; Forget, F.; Head, James W.; Levrard, B.; Montmessin, F.; Millour, E. (2009). "Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario". Icarus. 203 (2): 300–405. Bibcode:2009Icar..203..390M. doi:10.1016/j.icarus.2009.04.037. 
  27. ^ Mischna, M.; Richardson, Mark I.; Wilson, R. John; McCleese, Daniel J. (2003). "On the orbital forcing of martian water and CO2 cycles: A general circulation model study with simplified volatile schemes". J. Geophys. Res. 108 (E6): 5062. Bibcode:2003JGRE..108.5062M. doi:10.1029/2003JE002051. 
  28. ^ Parker, M.; et al. (2010). "3D structure of the Gusev Crater region". Earth and Planetary Science Letters. 294 (3–4): 411–423. Bibcode:2010E&PSL.294..411P. doi:10.1016/j.epsl.2010.01.013. 
  29. ^ Kreslavsky, M.; Head, J. (2006). "Modification of impact craters in the northern plains of Mars: Implications for the Amazonian climate history". Meteorit. Planet Sci. 41 (10): 1633–1646. Bibcode:2006M&PS...41.1633K. doi:10.1111/j.1945-5100.2006.tb00441.x. 
  30. ^ Rodríguez, Jose Alexis Palmero (2005). "Control of impact crater fracture systems on subsurface hydrology, ground subsidence, and collapse, Mars". Journal of Geophysical Research. 110. Bibcode:2005JGRE..11006003R. doi:10.1029/2004JE002365. 
  31. ^ Pedersen, G., J. Head. 2010. Chaos formation by sublimation of volatile-rich substrate: Evidence from Galaxias Chaos, Mars. Icarus: 211, 316–329.
  32. ^ Kreslavsky, Mikhail A.; Head, James W. (2002). "Fate of outflow channel effluents in the northern lowlands of Mars: The Vastitas Borealis Formation as a sublimation residue from frozen ponded bodies of water". Journal of Geophysical Research. 107: 5121. Bibcode:2002JGRE..107.5121K. doi:10.1029/2001JE001831. 
  33. ^ Carr, Michael H.; Head, James W. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate" (PDF). Journal of Geophysical Research. 108 (E5): 5042. Bibcode:2003JGRE..108.5042C. doi:10.1029/2002JE001963. 
  34. ^
  35. ^