Difference between revisions of "Sublimation landscapes on Mars"

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[[File:53642 2225brains.jpg |thumb|200px|left|Open and closed brain terrain]]
 
[[File:53642 2225brains.jpg |thumb|200px|left|Open and closed brain terrain]]
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[[File:45507 2200brains.jpg |thumb|200px|right|Brain terrain]]
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==Ribbed Terrain==
 
==Ribbed Terrain==

Revision as of 05:58, 23 May 2018

Due to the thin atmosphere and extreme cold on Mars, sublimation is very significant in creating Water ice to water vapor. There is much evidence that the Red Planet once held much water. It probably had streams, rivers, lakes, and perhaps an ocean.

Brain Terrain

Today, most of the water has left the planet, but a substantial amount is left frozen the ground and in a material called “latitude dependent mantle.” After cracks form in the frozen ground and mantle, the fun begins. The cracks greatly increase the surface area over which water can sublimate. Water sublimates and leaves behind dust. The dust can insulated the ground below from losing more water for a time or, at times the dust can be blown away. This process creates various holes and pits on the surface. A common feature in ice-rich ground is “brain terrain.” So named for its resemblance to the human brain. Sublimation is greatly increased along the surface of cracks.[1] In time, some broad ridges are left which may still contain some water-ice. The cracks form random patterns So the high and low points are random, thus looking like the outside of our brains. Initially the ridges are wide making what’s called “closed brain terrain;” later when ice leaves the core of the wide ridges, “open brain terrain” results.[2]

Open and closed brain terrain
Brain terrain

File:45507 2200brains.jpg

Ribbed Terrain

Sometimes large amounts of ice leave along the cracks and the cracks are bigger, but less in number. Eventually, wide canyons appear. This forms what has been called “ribbed terrain.”[3] A wide version of this sometimes forms wide canyons where the ground seems to be hollowed out. These places can be very beautiful.

  • Ribbed terrain Sublimation along narrow cracks cause ribbed terrain with wide troughs to form.

  • Hollowed terrain that developed from ribbed terrain. Sublimation along narrow cracks cause ribbed terrain with wide troughs to form.

  • Hollowed terrain Box shows the size of a football field. Sublimation along narrow cracks cause ribbed terrain with wide troughs to form.

Scalloped Terrain

Another form that develops in ice-rich ground, especially in the higher latitudes is what’s called “scalloped terrain.” It looks like material has been scooped out. Usually scalloped depressions have a steeper pole-facing wall and a gentle equator facing slope.[4]


  • Scalloped terrain The steep wall faces the north pole. Studies from orbit have shown the presence of ice in these formations.

  • Close view of Scalloped terrain in the Casius quadrangle The steep wall faces the north pole. Studies from orbit have shown the presence of ice in these formations.


Seasonal Changes

During the Martian winter dry ice is deposited at the winter pole. During the Martian summer carbon dioxide ice sublimes from the summer pole. The amount that is deposited and then sublimated in the spring is huge—indeed at least 12-16 % of the atmosphere is deposited and removed each Martian year.[5] [6] This process causes great pressure changes and high winds.

Spiders

In places at the southern pole, a thick slab of transparent dry ice covers the ground. With the arrival of higher sunlight levels, much sublimation occurs under the slab and builds up pressure. When cracks appear in weak areas, the gas rushes out at high speeds carrying black dust with it. Speeds may be up to 100 miles per hour.[7] These events can resemble terrestrial geysers. Often surface winds spread the black dust into a fan shaped plume. Under the ice, channels frequently form which looks like a spider, so they are named “spiders.”

Spiders indicated with arrows. The plume on the right was caused by wind blowing from the bottom to the top of the image.

Swiss Cheese Terrain

Also, in the southern area, “Swiss Cheese Terrain” develops. Pits form in a 1-10 meter thick layer of dry ice. They get larger and larger in are until the surface looks like Swiss cheese. They start along small fractures.[8] [9] [10] [11] [12]

Swiss cheese terrain, as seen by HiRISE

Gullies

In mid-latitudes, gullies are common in large areas in both the northern and southern hemisphere. They occur on steep slopes like crater walls.[13] [14] For many years, they were thought to be caused by running water. However, closer examination over a period of years revealed that some are growing under present conditions where liquid water is not possible.[15] Experiments on Earth demonstrated that chunks of dry ice moving down slopes could create gullies with a similar appearance. So, at least some of the gullies are being formed by dry ice building up in the winter and then causing erosion as they slide downhill in the warm spring.[16] [17] [18] This process is aided by carbon dioxide vapor jetting off the dry ice and lifting it a bit.[19] Note that present growth of gullies happens just as the temperature rises to where dry ice can easily sublimate.

  • Gullies along mesa wall in Arcadia quadrangle

  • Gullies along a steep slope

See also

References

  1. ↑ Mangold, N (2003). "Geomorphic analysis of lobate debris aprons on Mars at Mars Orbiter Camera scale: Evidence for ice sublimation initiated by fractures." J. Geophys. Res. 108: 8021.
  2. ↑ Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.
  3. ↑ Baker, D., J. Head. 2015. Extensive Middle Amazonian mantling of debris aprons and plains in Deuteronilus Mensae, Mars: Implication for the record of mid-latitude glaciation. Icarus: 260, 269-288.
  4. ↑ Lefort, A.; Russell, P. S.; Thomas, N.; McEwen, A. S.; Dundas, C. M.; Kirk, R. L. (2009). "Observations of periglacial landforms in Utopia Planitia with the High Resolution Imaging Science Experiment (HiRISE)". Journal of Geophysical Research. 114 (E4)
  5. ↑ Antonio Genova, Sander Goossens, Frank G. Lemoine, Erwan Mazarico, Gregory A. Neumann, David E. Smith, Maria T. Zuber. Seasonal and static gravity field of Mars from MGS, Mars Odyssey and MRO radio science. Icarus, 2016; 272: 228 DOI: 10.1016/j.icarus.2016.02.05
  6. ↑ NASA/Goddard Space Flight Center. "New gravity map gives best view yet inside Mars." ScienceDaily. ScienceDaily, 21 March 2016.
  7. ↑ http://themis.asu.edu/news/gas-jets-spawn-dark-spiders-and-spots-mars-icecap
  8. ↑ Thomas,P., M. Malin, P. James, B. Cantor, R. Williams, P. Gierasch South polar residual cap of Mars: features, stratigraphy, and changes Icarus, 174 (2 SPEC. ISS.). 2005. pp. 535–559. http://doi.org/10.1016/j.icarus.2004.07.028
  9. ↑ Thomas, P., P. James, W. Calvin, R. Haberle, M. Malin. 2009. Residual south polar cap of Mars: stratigraphy, history, and implications of recent changes Icarus: 203, 352–375 http://doi.org/10.1016/j.icarus.2009.05.014
  10. ↑ Thomas, P., W.Calvin, P. Gierasch, R. Haberle, P. James, S. Sholes. 2013. Time scales of erosion and deposition recorded in the residual south polar cap of mars Icarus: 225: 923–932 http://doi.org/10.1016/j.icarus.2012.08.038
  11. ↑ Thomas, P., W. Calvin, B. Cantor, R. Haberle, P. James, S. Lee. 2016. Mass balance of Mars’ residual south polar cap from CTX images and other data Icarus: 268, 118–130 http://doi.org/10.1016/j.icarus.2015.12.03
  12. ↑ Buhler, Peter, Andrew Ingersoll, Bethany Ehlmann, Caleb Fassett, James Head. 2017. How the martian residual south polar cap develops quasi-circular and heart-shaped pits, troughs, and moats. Icarus: 286, 69-9.
  13. ↑ Malin, M.; Edgett, K. (2000). "Evidence for recent groundwater seepage and surface runoff on Mars". Science. 288: 2330–2335
  14. ↑ Edgett, K.; et al. (2003). "Polar-and middle-latitude martian gullies: A view from MGS MOC after 2 Mars years in the mapping orbit" (PDF). Lunar Planet. Sci. 34. Abstract 1038.
  15. ↑ https://scitechdaily.com/linear-gullies-on-mars-caused-by-sliding-dry-ice
  16. ↑ http://www.psrd.hawaii.edu/Aug03/MartianGullies.html
  17. ↑ Diniega, S.; Byrne, S.; Bridges, N. T.; Dundas, C. M.; McEwen, A. S. (2010). "Seasonality of present-day Martian dune-gully activity". Geology. 38: 1047–1050.
  18. ↑ NASA/Jet Propulsion Laboratory. "Study links fresh Mars gullies to carbon dioxide." ScienceDaily 30 October 2010. 10 March 2011
  19. ↑ https://www.nasa.gov/home/hqnews/2013/jun/HQ_13-180_Mars_Dry_Ice_Gullies.html#.WXDOT4WcGUk

External links

  • [[1]] Video demonstrates how dry ice can form gullies on dunes
  • APOD |date=21 February 2003|title=Melting Snow and the Gullies of Mars
  • APOD |date=17 June 2013|title=Dry Ice Sled Streaks on Mars
  • VEDIE et al., 2008 : Laboratory simulations of martian gullies on the Russel crater sand dunes http://www.agu.org/pubs/crossref/2008/2008GL035638.shtml
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