Layers on Mars - Revision history

Suitupshowup: /* Inside craters */ added image

2024-01-02T17:23:20Z

Inside craters: added image

Suitupshowup: /* Inside craters */

2023-09-11T22:11:29Z

Inside craters

Suitupshowup: /* Inside craters */

2023-09-11T22:10:37Z

Inside craters

Suitupshowup: /* Inside craters */ added image

2023-09-11T22:09:42Z

Inside craters: added image

Suitupandshowup: /* Mantle layers */ added ref

2020-12-26T16:18:43Z

Mantle layers: added ref

Michel Lamontagne at 14:50, 13 November 2020

2020-11-13T14:50:22Z

Suitupandshowup: /* Along ancient river valleys */

2020-04-16T16:39:22Z

Along ancient river valleys

Suitupandshowup: /* External links */ added link

2020-03-23T12:47:52Z

External links: added link

Suitupandshowup: /* Recommended reading */ addd link

2020-03-23T12:29:16Z

Suitupandshowup at 21:24, 9 March 2020

2020-03-09T21:24:51Z

@@ Line 97: / Line 97: @@
 File:Wikiesp 035896 1845crommelinhollows.jpg|Layered mound on floor of Crommelin Crater
 File:53289 1845layers2faultcrommelin.jpg|Layers in Crommelin Crater  Arrow indicates a fault.
 </gallery>
 ==Mantle layers==

@@ Line 92: / Line 92: @@
 File:Layered mound in Firsoff Crater, Mars 79401 1820layeredmoundfirsoff 03.jpg|Layered mound in Firsoff Crater
 </gallery>
 <gallery class="center"  widths="380px" heights="360px">
 File:Henry Crater Mound.JPG|Layers exposed on mound in Henry Crater

@@ Line 90: / Line 90: @@
 <gallery class="center"  widths="380px" heights="360px">
-File:Layered mound in Firsoff Crater, Mars 79401 1820layeredmoundfirsoff 03.jpg
+File:Layered mound in Firsoff Crater, Mars 79401 1820layeredmoundfirsoff 03.jpg|Layered mound in Firsoff Crater
 </gallery>
 <gallery class="center"  widths="380px" heights="360px">

@@ Line 88: / Line 88: @@
 Layers in Firsoff Crater, as seen by HiRISE under HiWish program
 <gallery class="center"  widths="380px" heights="360px">
 File:Henry Crater Mound.JPG|Layers exposed on mound in Henry Crater

@@ Line 97: / Line 97: @@
 ==Mantle layers==
-Another class of layers may have been created as ice-rich material fell from the sky when the climate changed.  Because Mars has no large moon to stabilize its tilt, its tilt, and thus its climate vary greatly.  At times moisture from the poles enters the atmosphere, and freezes to form snow or ice-coatcoated dust.  This ice-rich material collects at mid latitudes.  It appears as a smooth covering, called latitude dependent mantle.  After each climate change, some of the material stays behind, while much just returns to the Polar Regions.  This repeated process results in layers in craters and in sheltered spots like against cliffs.  Some of these formations have been shaped by the wind into various shapes.
+Another class of layers may have been created as ice-rich material fell from the sky when the climate changed.  Because Mars has no large moon to stabilize its tilt, its tilt, and thus its climate vary greatly.<ref>https://www.uahirise.org/hipod/ESP_034132_1750</ref>  At times moisture from the poles enters the atmosphere, and freezes to form snow or ice-coatcoated dust.  This ice-rich material collects at mid latitudes.  It appears as a smooth covering, called latitude dependent mantle.  After each climate change, some of the material stays behind, while much just returns to the Polar Regions.  This repeated process results in layers in craters and in sheltered spots like against cliffs.  Some of these formations have been shaped by the wind into various shapes.
 It must be pointed out that mantle is widespread on Mars and contains water ice.  This ice can be a major source of water for future colonists.

← Older revision		Revision as of 14:50, 13 November 2020
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		+	{{Mars atlas}}
	Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.		Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.

@@ Line 32: / Line 32: @@
 File:Shalbatana Vallis.JPG|Layers in wall of Shalbatana Vallis
-ESP 048980 1725layers.jpg|Wide view of layers in [[Louros Valles]], as seen by HiRISE under HiWish program  Louros Valles is part of the [[Ius Chasma]].
+ESP 048980 1725layers.jpg|Wide view of layers in Louros Valles, as seen by HiRISE under HiWish program  Louros Valles is part of the Ius Chasma.
 1725layersclose2.jpg|Close view of layers in Louros Valles  Note this is an enlargement of a previous image.

← Older revision		Revision as of 12:47, 23 March 2020
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	*[https://www.uahirise.org/PSP_007820_1505 Layered Sediments in Hellas Planitia]		*[https://www.uahirise.org/PSP_007820_1505 Layered Sediments in Hellas Planitia]
		+
		+	*[https://www.youtube.com/watch?v=RYG-HLr33CM Jim Secosky - Martian Geology - 16th Annual International Mars Society Convention]

	[[Category: Geologic Processes]]		[[Category: Geologic Processes]]

← Older revision		Revision as of 12:29, 23 March 2020
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	* Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.		* Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
		+
		+	== External links ==
		+
		+	*[https://www.uahirise.org/PSP_007820_1505 Layered Sediments in Hellas Planitia]

	[[Category: Geologic Processes]]		[[Category: Geologic Processes]]

@@ Line 7: / Line 7: @@
 Layers show up in the walls of craters.
-<gallery class="center"  widths="190px" heights="180px">
+<gallery class="center"  widths="380px" heights="360px">
 File: 57080 1380layerscratercolor.jpg|Layers in crater wall in Phaethontis quadrangle, as seen by HiRISE under HiWish program
 File:ESP 057098 2050layers.jpg|Layers around crater in Syrtis Major quadrangle
@@ Line 16: / Line 16: @@
 Mars has spectular canyons and troughs where the ground has pulled apart due to the stress caused by the weight of giant volcanoes.  In these places layers often run continually for long distances.
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 Image:Noctis Labyrinthusmgs.jpg|Close view of layers in Noctis Labyrinthus
@@ Line 29: / Line 29: @@
 Many features resemble long river valleys similar to what is common on the Earth.  Layering occurs along many of the walls.
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:Shalbatana Vallis.JPG|Layers in wall of Shalbatana Vallis
@@ Line 44: / Line 44: @@
 Mesas and pedestal craters, a feature unique to Mars, often show layers.  Both of these are the remains of layers that once covered wide regions.  They often owe their existence to an erosion-resistant top layer.  Sometimes it is from a layer of hard lava that covered everything.  Cap rock, a name given to this hard layer, is seen to break into large blocks or boulders in some cap rocks.
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:Wikiesp 035896 1845crommelinbutte.jpg|Layers in Crommelin Crater
 File:47080 2120layersclose.jpg|Layers in mesa in Mare Acidalium quadrangle
@@ Line 52: / Line 52: @@
 Pedestal craters develop a protective top layer from the action of crater ejecta.
 File:ESP 047367 1910pedestal.jpg|Wide view of pedestal    The  southern  (lower) edge is enlarged in next image to show layers.
 File:47367 1910pedestallayerssouth.jpg|Close view of layers in pedestal crater in Arabia quadrangle
@@ Line 63: / Line 63: @@
 The insides of many craters contain layered deposits.  They appear to have formed sometime after the crater was blasted into the surface.  The Mars Curiosity Rover was sent to examine one of these formations.  It quickly found rounded pebbles–strong evidence for running water. <ref>  https://www.nasa.gov/home/hqnews/2012/sep/HQ_12-338_Mars_Water_Stream.html</ref>  <ref>https://www.youtube.com/watch?v=fYo31XjoXOk  </ref>  <ref>http://apnews.excite.com/article/20120927/DA1IDOO00.html  </ref>  Later, it was determined that indeed Gale Crater once held a lake. <ref>https://www.nasa.gov/press/2014/december/nasa-s-curiosity-rover-finds-clues-to-how-water-helped-shape-martian-landscape </ref>    <ref>https://www.sciencedaily.com/releases/2014/12/141208122903.htm  </ref>   <ref> https://www.jpl.nasa.gov/video/details.php?id=1346 </ref>   <ref>https://www.jpl.nasa.gov/news/news.php?feature=4398</ref> The lake in Gale, became full of sediments.  Later, all but the center mound was eroded.  However, there are other ideas that have been considered for the origin of Gale's mound.<ref>http://science.sciencemag.org/content/363/6426/535.full?ijkey=xakdRhWj7CWEE&keytype=ref&siteid=sci</ref> <ref>https://www.jpl.nasa.gov/news/news.php?feature=7323</ref> <ref>http://science.sciencemag.org/content/363/6426/535.abstract?ijkey=xakdRhWj7CWEE&keytype=ref&siteid=sci</ref> <ref>Lewis, K., et al.  2019.  A surface gravity traverse on Mars indicates low bedrock density at Gale crater.  Science: 363, 535-537.</ref>
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:PIA16105 malin04ano-br2.jpg|Layers at base of Mount Sharp, the mound in Gale crater, as seen by Curiosity's  Mast Camera  The insert shows a rock about the size of Curiosity.
@@ Line 72: / Line 72: @@
 Many other past lakes have been proposed for craters and other low regions.<ref>De Hon, R. 1992. Martian lake basins and lacustrine plains. Earth Moon Planets: 56, 95-122.</ref> <ref>Cabrol, N., E. Grin. 1999. Distribution, classification, and ages of martian impact crater lakes. Icarus: 142, 160-172.</ref> <ref>Cabrol, N., E. Grin. 2001. The evolution of lacustrine environments on Mars: Is Mars only hydrologically dormant. Icarus: 149, 291-328</ref> <ref>Goudge, T., K. Aureli, J. Head, C. Fassett, J. Mustard. 2015. Classification and analysis of candidate impact crater-hosted closed-basin lakes on Mars. Icarus: 260, 346-367.</ref><ref>Fassett, C. J. Head. 2008. Valley network-fed, open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology. Icarus: 198, 37-56.</ref> <ref>Zhao, J., et al. 2018. PALEOLAKES IN THE NORTHWEST HELLAS REGION: IMPLICATIONS FOR PALEO-CLIMATE AND REGIONAL GEOLOGIC HISTORY. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).</ref>
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:56836 1900layedmound2.jpg|Layers on crater floor in Arabia quadrangle
 File:56836 1900layedmoundfootball.jpg|Layers on crater floor, as seen by HiRISE under HiWish program  Box shows size of a football field.
@@ Line 88: / Line 88: @@
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:Henry Crater Mound.JPG|Layers exposed on mound in Henry Crater
 File:Wikiesp 035896 1845crommelinhollows.jpg|Layered mound on floor of Crommelin Crater
@@ Line 99: / Line 99: @@
 It must be pointed out that mantle is widespread on Mars and contains water ice.  This ice can be a major source of water for future colonists.
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:ESP 050793 1365pyramids.jpg| Wide view of layered features in Hellas quadrangle
 File:50793 1365layers2.jpg|Close view of layered features in Hellas quadrangle   Each layer may represent a change in the climate.
@@ Line 108: / Line 108: @@
 We have known about layers in the northern ice cap for a long time.  They record many past climate changes.
-<gallery class="center" widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 File:ESP 044934 2670icecaplayers.jpg|Layers exposed in ice cap in Mare Boreum quadrangle
 File:ESP 036863 2670icecaplayers.jpg| Layers exposed in ice cap in Mare Boreum quadrangle