Amenthes quadrangle

Amenthes quadrangle

Map of Amenthes quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
Coordinates 15°00′N 247°30′W / 15°N 247.5°W / 15; -247.5Coordinates: 15°00′N 247°30′W / 15°N 247.5°W / 15; -247.5
Image of the Amenthes Quadrangle (MC-14). The southern part includes heavily cratered highlands; the northern part contains Elysium Planitia; and, the eastern half includes Isidis basin.

The Amenthes quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Amenthes quadrangle is also referred to as MC-14 (Mars Chart-14).[1] The quadrangle covers the area from 225° to 270° west longitude and from 0° to 30° north latitude on Mars. Amenthes quadrangle contains parts of Utopia Planitia, Isidis Planitia, Terra Cimmeria, and Tyrrhena Terra.

This quadrangle contains the Isidis basin, a location where magnesium carbonate was found by MRO. This mineral indicates that water was present and that it was not acidic. There are Dark slope streaks, troughs (fossae), and river valleys (Vallis) in this quadrangle.

The Beagle 2 lander was about to land in the quadrangle, particularly in the eastern part of Isidis Planitia, in December 2003, when contact with the craft was lost. In January 2015, NASA reported the Beagle 2 had been found on the surface in Isidis Planitia (location is about 11°31′35″N 90°25′46″E / 11.5265°N 90.4295°E / 11.5265; 90.4295).[2][3] High-resolution images captured by the Mars Reconnaissance Orbiter identified the lost probe, which appears to be intact.[4][5][6] (see discovery images here)

Craters

Some craters in the Amenthes region (as well as other parts of Mars) show ejecta around them that have lobes. It is believed that the lobed shape is caused by an impact into water or ice logged ground. Calculations suggest that ice is stable beneath the Martian surface.

At the equator the stable layer of ice might lie under as much as 1 kilometer of material, but at higher latitudes the ice may be just a few centimeters below the surface. This was proven when the landing rockets on the Phoenix lander blew away surface dust to reveal an ice surface.[7][8] The larger an impact crater, the deeper its penetration, a large crater is more likely to have a lobate ejecta since it went down to the ice layer. When even small craters have lobes, the ice level is close to the surface.[9] This idea would be very important for future colonists on Mars who would like to live near a source of water.

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.[10] 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.

Why are Craters important?

The density of impact craters is used to determine the surface ages of Mars and other solar system bodies.[11] The older the surface, the more craters present. Crater shapes can reveal the presence of ground ice.

The area around craters may be rich in minerals. On Mars, heat from the impact melts ice in the ground. Water from the melting ice dissolves minerals, and then deposits them in cracks or faults that were produced with the impact. This process, called hydrothermal alteration, is a major way in which ore deposits are produced. The area around Martian craters may be rich in useful ores for the future colonization of Mars.[12] Studies on the earth have documented that cracks are produced and that secondary minerals veins are deposited in the cracks.[13][14][15] Images from satellites orbiting Mars have detected cracks near impact craters.[16] Great amounts of heat are produced during impacts. The area around a large impact may take hundreds of thousands of years to cool.[17][18][19] Many craters once contained lakes.[20][21][22] Because some crater floors show deltas, we know that water had to be present for some time. Dozens of deltas have been spotted on Mars.[23] Deltas form when sediment is washed in from a stream entering a quiet body of water. It takes a bit of time to form a delta, so the presence of a delta is exciting; it means water was there for a time, maybe for many years. Primitive organisms may have developed in such lakes; hence, some craters may be prime targets for the search for evidence of life on the Red Planet.[24]

Hebrus Valles

Hebrus Vales has tributaries, terraces, and teardrop shaped islands. The tear drop shape of the islands indicate what direction the water used to flow. The terraces may be caused by different layers of rocks or from the water being at different levels.[25] These features are common for the rivers of the Earth.

Streamlined shapes

Streamlined shapes are formed from erosion by flowing water.

Gallery

Other Mars quadrangles

Interactive Mars map

Acidalia Planitia Acidalia Planitia Alba Mons Amazonis Planitia Aonia Terra Arabia Terra Arcadia Planitia Arcadia Planitia Argyre Planitia Elysium Mons Elysium Planitia Hellas Planitia Hesperia Planum Isidis Planitia Lucas Planum Lyot (crater) Noachis Terra Olympus Mons Promethei Terra Rudaux (crater) Solis Planum Tempe Terra Terra Cimmeria Terra Sabaea Terra Sirenum Tharsis Montes Utopia Planitia Valles Marineris Vastitas Borealis Vastitas BorealisMap of Mars
Interactive imagemap of the global topography of Mars. Hover your mouse to see the names of over 25 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Reds and pinks are higher elevation (+3 km to +8 km); yellow is 0 km; greens and blues are lower elevation (down to −8 km). Whites (>+12 km) and browns (>+8 km) are the highest elevations. Axes are latitude and longitude; Poles are not shown.
(view • discuss)

See also

References

  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. ↑ Ellison, Doug (16 January 2015). "re Beagle 2 location on Mars => "Using HiView on image ESP_039308_1915_COLOR.JP2 I get 90.4295E 11.5265N"". Twitter & JPL. Retrieved 19 January 2015.
  3. ↑ Grecicius, Tony; Dunbar, Brian (16 January 2015). "Components of Beagle 2 Flight System on Mars". NASA. Retrieved 18 January 2015.
  4. ↑ Webster, Guy (16 January 2015). "'Lost' 2003 Mars Lander Found by Mars Reconnaissance Orbiter". NASA. Retrieved 16 January 2015.
  5. ↑ Associated Press (16 January 2015). "Mars Orbiter Spots Beagle 2, European Lander Missing Since 2003". New York Times. Retrieved 17 January 2015.
  6. ↑ Amos, Jonathan (16 January 2015). "Lost Beagle2 probe found 'intact' on Mars". BBC. Retrieved 16 January 2015.
  7. ↑ http://www.nasa.gov/mission_pages/phoenix/news/phoenix-20080531.html
  8. ↑ http://www.nasa.gov/centers/ames/news/releases/2008/08_108AR_prt.html
  9. ↑ http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31026
  10. ↑ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011.
  11. ↑ http://www.lpi.usra.edu/publications/slidesets/stones/
  12. ↑ http://www.indiana.edu/~sierra/papers/2003/Patterson.html.
  13. ↑ Osinski, G, J. Spray, and P. Lee. 2001. Impact-induced hydrothermal activity within the Haughton impact structure, arctic Canada: Generation of a transient, warm, wet oasis. Meteoritics & Planetary Science: 36. 731-745
  14. ↑ http://www.ingentaconnect.com/content/arizona/maps/2005/00000040/00000012/art00007
  15. ↑ Pirajno, F. 2000. Ore Deposits and Mantle Plumes. Kluwer Academic Publishers. Dordrecht, The Netherlands
  16. ↑ Head, J. and J. Mustard. 2006. Breccia Dikes and Crater-Related Faults in Impact Craters on Mars: Erosion and Exposure on the Floor of a 75-km Diameter Crater at the Dichotomy Boundary. Special Issue on Role of Volatiles and Atmospheres on Martian Impact Craters Meteoritics & Planetary Science
  17. ↑ name="news.discovery.com"
  18. ↑ Segura, T, O. Toon, A. Colaprete, K. Zahnle. 2001. Effects of Large Impacts on Mars: Implications for River Formation. American Astronomical Society, DPS meeting#33, #19.08
  19. ↑ Segura, T, O. Toon, A. Colaprete, K. Zahnle. 2002. Environmental Effects of Large Impacts on Mars. Science: 298, 1977-1980.
  20. ↑ Cabrol, N. and E. Grin. 2001. The Evolution of Lacustrine Environments on Mars: Is Mars Only Hydrologically Dormant? Icarus: 149, 291-328.
  21. ↑ Fassett, C. and J. Head. 2008. Open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology. Icarus: 198, 37-56.
  22. ↑ Fassett, C. and J. Head. 2008. Open-basin lakes on Mars: Implications of valley network lakes for the nature of Noachian hydrology.
  23. ↑ Wilson, J. A. Grant and A. Howard. 2013. INVENTORY OF EQUATORIAL ALLUVIAL FANS AND DELTAS ON MARS. 44th Lunar and Planetary Science Conference.
  24. ↑ Newsom H. , Hagerty J., Thorsos I. 2001. Location and sampling of aqueous and hydrothermal deposits in martian impact craters. Astrobiology: 1, 71-88.
  25. ↑ http://themis.asu.edu/zoom-20020603a
  26. 1 2 Morton, Oliver (2002). Mapping Mars: Science, Imagination, and the Birth of a World. New York: Picador USA. p. 98. ISBN 0-312-24551-3.
  27. ↑ "Online Atlas of Mars". Ralphaeschliman.com. Retrieved December 16, 2012.
  28. ↑ "PIA03467: The MGS MOC Wide Angle Map of Mars". Photojournal. NASA / Jet Propulsion Laboratory. February 16, 2002. Retrieved December 16, 2012.
  29. ↑ "Online Atlas of Mars". Ralphaeschliman.com. Retrieved December 16, 2012.
  30. ↑ "PIA03467: The MGS MOC Wide Angle Map of Mars". Photojournal. NASA / Jet Propulsion Laboratory. February 16, 2002. Retrieved December 16, 2012.

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