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Amenthes quadrangle
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Amenthes quadrangle : ウィキペディア英語版
Amenthes quadrangle

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).〔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.〕 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 ). High-resolution images captured by the Mars Reconnaissance Orbiter identified the lost probe, which appears to be intact. (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.〔http://www.nasa.gov/mission_pages/phoenix/news/phoenix-20080531.html〕〔http://www.nasa.gov/centers/ames/news/releases/2008/08_108AR_prt.html〕 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.〔http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31026〕 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. 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.

Image:Escalante Crater Wall.JPG|Escalante Crater wall, as seen by HiRISE. Image on left is an enlargement.
Image:Onon Crater.JPG|Onon Crater, as seen by HiRISE. Scale bar is 500 meters long.
Image:Libya Montes Region.JPG|Libya Montes Region, as seen by HiRISE. Image contains some sheer rock cliffs.
Wikidumartheraywest.jpg|Western side of Du Martheray Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).


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