Aeolis quadrangle - Revision history

Suitupshowup at 15:52, 24 April 2026

2026-04-24T15:52:03Z

Suitupshowup: /* See also */ added link

2026-04-24T15:50:45Z

Suitupshowup at 14:15, 24 January 2025

2025-01-24T14:15:02Z

Suitupshowup: added image

2024-12-27T23:18:50Z

added image

Suitupshowup: /* Other features in Aeolis quadrangle */ added image

2024-04-11T13:14:30Z

Other features in Aeolis quadrangle: added image

Suitupshowup: /* External links */

2024-01-02T23:00:37Z

External links

Suitupshowup: /* External links */ added ref

2024-01-02T23:00:10Z

External links: added ref

Suitupshowup: /* Layered terrain as seen by HiRISE */

2023-12-24T23:02:30Z

Layered terrain as seen by HiRISE

Suitupshowup: /* Layered terrain as seen by HiRISE */

2023-12-24T23:01:19Z

Layered terrain as seen by HiRISE

Suitupshowup: /* Gale Crater */

2023-12-24T22:57:01Z

Gale Crater

@@ Line 314: / Line 314: @@
 *[[Columbus Crater]]
 *[[Curiosity]]
-*[[Gale crater]]
+*[[Gale Crater]]
 *[[Geography of Mars]]
 *[[High Resolution Imaging Science Experiment (HiRISE)]]

@@ Line 314: / Line 314: @@
 *[[Columbus Crater]]
 *[[Curiosity]]
 *[[Geography of Mars]]
 *[[High Resolution Imaging Science Experiment (HiRISE)]]

@@ Line 8: / Line 8: @@
 |}
-Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.<gallery widths="400" heights="300">
+Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.
 File:USGS-Mars-MC-23-AeolisRegion-mola.png|Labeled topo map of Aeolis quadrangle  Colors indicate elevation
 File:PIA00183-MC-23-AeolisRegion-19980605.jpg|Image of the Aeolis Quadrangle (MC-23). The northern part contains Elysium Planitia. The northeastern part includes Apollinaris Patera. The southern part mostly contains heavily cratered highlands.

← Older revision		Revision as of 23:18, 27 December 2024
Line 12:		Line 12:
	File:PIA00183-MC-23-AeolisRegion-19980605.jpg\|Image of the Aeolis Quadrangle (MC-23). The northern part contains Elysium Planitia. The northeastern part includes Apollinaris Patera. The southern part mostly contains heavily cratered highlands.		File:PIA00183-MC-23-AeolisRegion-19980605.jpg\|Image of the Aeolis Quadrangle (MC-23). The northern part contains Elysium Planitia. The northeastern part includes Apollinaris Patera. The southern part mostly contains heavily cratered highlands.
	</gallery>		</gallery>
		+
		+
		+
		+	[[File:Collage Aeolis 02.jpg\|Features of Features of Aeolis quadrangle, as seen by HiRISE under under HiWish program\|600pxr\| Features of Aeolis quadrangle]]
		+
		+	Scenes of the Aeolis quadrangle

@@ Line 296: / Line 296: @@
 File:Landslide from crater wall ESP 056712 1605.jpg|Landslide, this image was named HiRISE picture of the day for June 11, 2020
 </gallery>
 ==See also==

@@ Line 338: / Line 338: @@
 * http://global-data.mars.asu.edu/bin/ctx.pl For more CTX images
 * [https://www.youtube.com/watch?v=9rbnvdWk3eg The Lakes and Rivers of Ancient Mars]
 * Cousin, A., et al.  2017.  Classification of igneous rocks analyzed by ChemCam at Gale crater, Mars.  Icarus.
-Icarus.  Volume 288.  Pages 265-283.
+  Volume 288.  Pages 265-283.
 [[Category:Mars Atlas]]

@@ Line 250: / Line 250: @@
 Scientists were excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water.<ref>http://themis.asu.edu/features/nilosyrtis |title=Target Zone: Nilosyrtis? &#124; Mars Odyssey Mission THEMIS |publisher=Themis.asu.edu |</ref>  Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.<ref>http://hirise.lpl.arizona.edu/PSP_004046_2080 |title=HiRISE &#124; Craters and Valleys in the Elysium Fossae (PSP_004046_2080) |publisher=Hirise.lpl.arizona.edu </ref>
-Rock can form layers in a variety of ways.  Volcanoes, wind, or water can produce layers.<ref>http://hirise.lpl.arizona.edu?PSP_008437_1750 |title=HiRISE &#124; High Resolution Imaging Science Experiment |publisher=Hirise.lpl.arizona.edu?psp_008437_1750 |</ref>  Layers can be hardened by the action of groundwater.  Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through.  When ground water surfaces in low areas containing sediments, water evaporates into the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesed for Mars.  One location this occurs on Earth is the Great Artesian Basin of Australia.<ref>Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.</ref>  On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through.  Silica cement is very hard, while calcite is not as hard.
+Rock can form layers in a variety of ways.  Volcanoes, wind, or water can produce layers.<ref>http://hirise.lpl.arizona.edu?PSP_008437_1750 |title=HiRISE &#124; High Resolution Imaging Science Experiment |publisher=Hirise.lpl.arizona.edu?psp_008437_1750 |</ref>  Layers can be hardened by the action of groundwater.  Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through.  When ground water surfaces in low areas containing sediments, water evaporates into the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesed for Mars.  One location this occurs on Earth is the Great Artesian Basin of Australia.<ref>Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.</ref>  On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through.  Silica cement is very hard, while calcite is not as hard
@@ Line 272: / Line 265: @@
 [[File:47441 1800blocks.jpg|left|thumb|400px|Close view of blocks from a mesa Arrow shows a cube-shaped block that is the size of a house.]]
 ==Linear ridge networks==

@@ Line 251: / Line 251: @@
 Rock can form layers in a variety of ways.  Volcanoes, wind, or water can produce layers.<ref>http://hirise.lpl.arizona.edu?PSP_008437_1750 |title=HiRISE &#124; High Resolution Imaging Science Experiment |publisher=Hirise.lpl.arizona.edu?psp_008437_1750 |</ref>  Layers can be hardened by the action of groundwater.  Martian ground water probably moved hundreds of kilometers, and in the process it dissolved many minerals from the rock it passed through.  When ground water surfaces in low areas containing sediments, water evaporates into the thin atmosphere and leaves behind minerals as deposits and/or cementing agents. Consequently, layers of dust could not later easily erode away since they were cemented together. On Earth, mineral-rich waters often evaporate forming large deposits of various types of salts and other minerals. Sometimes water flows through Earth's aquifers, and then evaporates at the surface just as is hypothesed for Mars.  One location this occurs on Earth is the Great Artesian Basin of Australia.<ref>Habermehl, M. A. (1980) The Great Artesian Basin, Australia. J. Austr. Geol. Geophys. 5, 9–38.</ref>  On Earth the hardness of many sedimentary rocks, like sandstone, is largely due to the cement that was put in place as water passed through.  Silica cement is very hard, while calcite is not as hard.
-[[File: 51978 1720layers.jpg|left|thumb|400px|Layers]]
+File: 51978 1720layers.jpg|Layers
 [[File:ESP 039740 1730layeredpyramid.jpg|right|thumb|400px|Layered structure]]

@@ Line 173: / Line 173: @@
 [[File:7505 mars-curiosity-rover-gale-crater-beauty-shot-pia19839-full2.jpg|600pxr|View from the "Kimberley" formation on Mars taken by NASA's Curiosity rover.]]
-                                           View from the "Kimberley" formation on Mars taken by NASA's Curiosity rover.
+                  View from the "Kimberley" formation on Mars taken by NASA's Curiosity rover.
 [[File:7501 1750layersgale.jpg|600pxr|Layers in Gale Crater on the Western flank of Mt. Sharp]]
-                          Layers in Gale Crater on the Western flank of Mt. Sharp, as seen by HiRISE
+             Layers in Gale Crater on the Western flank of Mt. Sharp, as seen by HiRISE
@@ Line 203: / Line 203: @@
-              View from Mastcam on Curiosity showing sloping buttes and layered outcrops on lower Mount Sharp
+         View from Mastcam on Curiosity showing sloping buttes and layered outcrops on lower Mount Sharp
 ==Map of locations in Gale Crater==