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Elysium quadrangle

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Title: Elysium quadrangle  
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Elysium quadrangle

Elysium quadrangle
Map of Elysium quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
Coordinates
Image of the Elysium Quadrangle (MC-15). The north includes relatively smooth lowland plains. Elysium Mons and Albor Tholus are in the northwest and Orcus Patera is in the east.

The Elysium quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Elysium quadrangle is also referred to as MC-15 (Mars Chart-15).[1]

The Elysium quadrangle covers the area 180° to 225° west longitude and 0° to 30° north latitude on Mars. It contains major volcanoes named Elysium Mons and Albor Tholus and river valleys--one of which, Athabasca Valles may be one of the youngest on Mars. On the east side is an elongated depression called Orcus Patera.

Contents

  • Volcanoes 1
  • Layers 2
  • Fossae/pit craters 3
  • Methane 4
  • Craters 5
  • Vallis in the Elysium quadrangle 6
  • Gallery 7
  • See also 8
  • References 9

Volcanoes

The Elysium quadrangle contains the volcanoes Elysium Mons and Albor Tholus. Much of this area is covered with lava flows, some can even be shown approaching, then stopping upon reaching higher ground. (See pictures below for examples) Sometimes when lava flows the top cools quickly into a solid crust. However, the lava below often still flows, this action breaks up the top layer making it very rough.[2] Such rough flow is called aa.

Research, published in January 2010, described the discovery of a vast single lava flow, the size of the state of Oregon, that "was put in place turbulently over the span of several weeks at most."[3] This flow, near Athabasca Valles, is the youngest lava flow on Mars. It is thought to be of Late Amazonian Age.[4]

Layers

The Elysium Fossae contain layers, also called strata. Many places on Mars show rocks arranged in layers. Sometimes the layers are of different colors. Light-toned rocks on Mars have been associated with hydrated minerals like sulfates. The Mars Rover Opportunity examined such layers close-up with several instruments. Pictures taken from orbiting spacecraft show that some layers of rocks seem to break up into fine dust; consequently these rocks are probably composed of small particles. Other layers break up into large boulders, so they are probably much harder. Basalt, a volcanic rock, is thought comprise the layers that form boulders. Basalt has been identified on Mars in many places. Instruments on orbiting spacecraft have detected clay (also called phyllosilicates) in some layers. Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.[5] Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.[6]

Rock can be formed into layers in a variety of ways. Volcanoes, wind, or water can produce layers.[7]

Fossae/pit craters

The Elysium quadrangle is home to large troughs (long narrow depressions) called fossae in the geographical language used for Mars. Troughs are created when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. Fossae/pit craters are common near volcanoes in the Tharsis and Elysium system of volcanoes.[8] A trough often has two breaks with a middle section moving down, leaving steep cliffs along the sides; such a trough is called a graben.[9] New York State, is a lake that sits in a graben. Pits are produced when material collapses into the void that results from the stretching. Pit craters do not have rims or ejecta around them, like impact craters do. Studies have found that on Mars a fault may be as deep as 5 km, that is the break in the rock goes down to 5 km. Moreover, the crack or fault sometimes widens or dilates. This widening causes a void to form with a relatively high volume. When material slides into the void, a pit crater or a pit crater chain forms. On Mars, individual pit craters can join to form chains or even to form troughs that are sometimes scalloped.[10] Other ideas have been suggested for the formation of fossae and pit craters. There is evidence that they are associated with dikes of magma. Magma might move along, under the surface, breaking the rock, and more importantly melting ice. The resulting action would cause a crack to form at the surface. Pit craters are not common on Earth. Sinkholes, where the ground falls into a hole (sometimes in the middle of a town) resemble pit craters on Mars. However, on the Earth these holes are caused by subsurface limestone being dissolved, thereby causing a void.[10][11][12] The images below of the Cerberus Fossae, the Elysium Fossae and other troughs, as seen by HiRISE are examples of fossae.

Knowledge of the locations and formation mechanisms of pit craters and fossae is important for the future colonization of Mars because they may be reservoirs of water.[13]

Methane


  1. ^ Davies, M.E.; Batson, R.M.; Wu, S.S.C. “Geodesy and Cartography” in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars. University of Arizona Press: Tucson, 1992.
  2. ^ "Southern Margin of Cerberus Palus (PSP_010744_1840)". Retrieved 9 February 2009. 
  3. ^ http://www.jpl.nasa.gov/news/features.cfm?feature=2438
  4. ^ Jaeger, W. et al. 2010. Emplacement of the youngest flood lava on Mars: A short, turbulent story. Icarus: 205. 230-243.
  5. ^ http://themis.asu.edu/features/nilosyrtis
  6. ^ http://hirise.lpl.arizona.edu/PSP_004046_2080
  7. ^ http://hirise.lpl.arizona.edu?PSP_008437_1750
  8. ^ Skinner, J., L. Skinner, and J. Kargel. 2007. Re-assessment of Hydrovolcanism-based Resurfacing within the Galaxias Fossae Region of Mars. Lunar and Planetary Science XXXVIII (2007)
  9. ^ http://hirise.lpl.arizona.edu/PSP_008641_2105
  10. ^ a b Wyrick, D., D. Ferrill, D. Sims, and S. Colton. 2003. Distribution, Morphology and Structural Associations of Martian Pit Crater Chains. Lunar and Planetary Science XXXIV (2003)
  11. ^ http://www.swri.edu/4org/d20/DEMPS/planetgeo/planetmars.html
  12. ^ http://www.msss.com/mars_images/moc/2004/01/29/index.html
  13. ^ Ferrill, D., D. Wyrick, A. Morris, D. Sims, and N. Franklin. 2004. Dilational fault slip and pit chain formation on Mars 14:10:4-12
  14. ^ http://www.space.com/scienceastronomy/mars-methane-gas-disappears-quickly-100920.html
  15. ^ Allen, C., D. Oehler, and E. Venechuk. Prospecting for Methane in Arabia Terra, Mars - First Results. Lunar and Planetaary Science XXXVII (2006). 1193.pdf-1193.pdf.
  16. ^ http://www.spaceref.com:80/news/viewpr.html?pid=28914
  17. ^ http://www.lpi.usra.edu/publications/slidesets/stones/
  18. ^ Hugh H. Kieffer (1992). Mars. University of Arizona Press.  
  19. ^ Tornabene, L. et al. 2012. Widespread crater-related pitted materials on Mars. Further evidence for the role of target volatiles during the impact process. Icarus. 220: 348-368.
  20. ^ Christiansen, E. 1989. Lahars in the Elysium region of Mars. Geology. 17: 203-206.
  21. ^ Michael H. Carr (2006). The surface of Mars. Cambridge University Press.  
  22. ^ Cabrol, N. and E. Grin (eds.). 2010. Lakes on Mars. Elsevier. NY
  23. ^ Burr, D. et al. 2002. Repeated aqueous flooding from the Cerberus Fossae: evidence for very recently extant deep groundwater on Mars. Icarus. 159: 53-73.
  24. ^ "Feature Image: Floods in Athabasca Valles". Retrieved 9 February 2009. 
  25. ^ Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY NY.

References

See also

Gallery

Perhaps the youngest outflow channel on Mars is Athabasca Valles. It lies 620 miles southeast of the large volcano Elysium Mons. Athabasca was formed by water that burst out of Cerberus Fossae, a set of cracks or fissures in the ground.[22] [23] Cerberus Fossae most likely was formed from the stress on the crust caused by the weight of both Elysium Mons and Tharsis volcanoes. Current evidence suggests that Cerberus floods probably erupted in several stages.[24] Near the start of these channels (Cerberus Fossae), the system is called Athabasca Valles, to the south and east it is called Marte Vallis. Flow rates in Marte Vallis have been estimated at around 100 times that of the Mississippi River. Eventually, the system just seems to fade out in the plains of Amazonis Planitia.[25]

Some of the valleys in the Elysium quadrangle seem to start from grabens. Granicus Vallis and Tinjar Vallis begin at a graben that lies just to the west of Elysium Mons. Certain observations suggest that they may have been the location of lahars (mudflows). The graben may have formed because of volcanic dikes. Heat from the dikes would have melted a great deal of ice.[20] Two valleys, Hephaestus Fossae and Hebrus Valles, have sections that join and branch at high angles.[21]

Vallis in the Elysium quadrangle

Research published in the journal Icarus has found pits in Zunil Crater that are caused by hot ejecta falling on ground containing ice. The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.[19] Zunil crater as seen by THEMIS.

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak.[17] The peak is caused by a rebound of the crater floor following the impact.[18] Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed unto the surface. Hence, craters can show us what lies deep under the surface.

Craters

[16]

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