Amazonis quadrangle - Revision history

Suitupshowup: /* Medusae Fossae Formation */ added ref

2026-01-26T13:38:31Z

Medusae Fossae Formation: added ref

Suitupshowup at 16:10, 24 January 2025

2025-01-24T16:10:58Z

Suitupshowup: added image

2025-01-24T14:23:07Z

added image

Suitupshowup: /* More images from Amazonis quadrangle */ added image

2024-04-11T17:40:15Z

More images from Amazonis quadrangle: added image

Suitupshowup: /* Dark slope streaks */ added images

2024-01-14T17:55:26Z

Dark slope streaks: added images

Suitupshowup: /* Streamlined shapes */

2023-12-23T22:16:39Z

Streamlined shapes

Suitupshowup: /* Streamlined shapes */ added image

2023-12-23T20:28:04Z

Streamlined shapes: added image

Suitupshowup: /* Streamlined shapes */ added image

2023-12-23T20:23:47Z

Streamlined shapes: added image

Suitupshowup: /* Streamlined shapes */

2023-12-23T18:00:08Z

Streamlined shapes

Suitupshowup: /* Dark Slope Streaks */

2023-12-23T17:59:38Z

Dark Slope Streaks

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 ==Medusae Fossae Formation==
-The Amazonis quadrangle is of great interest to scientists because it contains a major part of a formation, called the Medusae Fossae Formation. This unit is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars. The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs. These ridges generally point in direction of the prevailing winds that carved them and demonstrate the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles,<ref>Grotzinger, J. and R. Milliken (eds.)  2012.  Sedimentary Geology of Mars.  SEPM</ref> and was most likely formed by the deposition of wind-blown dust or volcanic ash. Using a global climate model, a group of researchers concluded that the Medusae Fossae Formation could have easily been formed from ash from the volcanoes Apollinaris Mons, Arsia Mons, and possibly from Pavonis Mons.<ref>Kerber L., et al.  2012.  The disporsal of pyroclasts from ancient explosive volcanoes on Mars:  Implications for the friable layered deposits.  Icarus.  219:358-381.</ref>  Another evidence for a fine-grained composition is that the area gives almost no radar return.  For this reason it has been called a "stealth" region.<ref>ISBN 978-0-521-85226-5</ref>   Layers are seen in parts of the formation.  Images from spacecraft show that they have different degrees of hardness probably because of significant variations in the physical properties, composition, particle size, and/or cementation. Very few impact craters are visible throughout the area so the surface is relatively young.<ref>http://themis.asu.edu/zoom-20020416a</ref>   Researchers found that nearly all the dust that falls out of the atmosphere and that coats everything on Mars has its origin in the Medusae Fossae formation.<ref>http://redplanet.asu.edu/?tag=medusae-fossae-formation</ref>  It turns out that the chemical elements (sulfur and chlorine) in this formation, in the atmosphere, and covering the surface are the same.   The amount of dust on Mars is sufficient to form a 2 to 12 meters thick layer over the entire planet.<ref>https://www.sciencedaily.com/releases/2018/07/180724120854.htm</ref> <ref>Lujendra Ojha, Kevin Lewis, Suniti Karunatillake, Mariek Schmidt. The Medusae Fossae Formation as the single largest source of dust on Mars. Nature Communications, 2018; 9 (1) DOI: 10.1038/s41467-018-05291-5</ref>  Since there are relatively few depositional features in the Medusae Fossae Formation, most of the materials being eroded are probably small enough to be suspended in the atmosphere and transported long distances.<ref>Tanaka, K. L. Dust and ice deposition in the Martian geologic record. Icarus 144, 254–266 (2000).</ref>
+The Amazonis quadrangle is of great interest to scientists because it contains a major part of a formation, called the Medusae Fossae Formation. This unit is a soft, easily eroded deposit that extends for nearly 1,000 km along the equator of Mars. The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs. These ridges generally point in direction of the prevailing winds that carved them and demonstrate the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles.<ref>https://www.uahirise.org/hipod/ESP_046504_1785</ref> <ref>Grotzinger, J. and R. Milliken (eds.)  2012.  Sedimentary Geology of Mars.  SEPM</ref> and was most likely formed by the deposition of wind-blown dust or volcanic ash. Using a global climate model, a group of researchers concluded that the Medusae Fossae Formation could have easily been formed from ash from the volcanoes Apollinaris Mons, Arsia Mons, and possibly from Pavonis Mons.<ref>Kerber L., et al.  2012.  The disporsal of pyroclasts from ancient explosive volcanoes on Mars:  Implications for the friable layered deposits.  Icarus.  219:358-381.</ref>  Another evidence for a fine-grained composition is that the area gives almost no radar return.  For this reason it has been called a "stealth" region.<ref>ISBN 978-0-521-85226-5</ref>   Layers are seen in parts of the formation.  Images from spacecraft show that they have different degrees of hardness probably because of significant variations in the physical properties, composition, particle size, and/or cementation. Very few impact craters are visible throughout the area so the surface is relatively young.<ref>http://themis.asu.edu/zoom-20020416a</ref>   Researchers found that nearly all the dust that falls out of the atmosphere and that coats everything on Mars has its origin in the Medusae Fossae formation.<ref>http://redplanet.asu.edu/?tag=medusae-fossae-formation</ref>  It turns out that the chemical elements (sulfur and chlorine) in this formation, in the atmosphere, and covering the surface are the same.   The amount of dust on Mars is sufficient to form a 2 to 12 meters thick layer over the entire planet.<ref>https://www.sciencedaily.com/releases/2018/07/180724120854.htm</ref> <ref>Lujendra Ojha, Kevin Lewis, Suniti Karunatillake, Mariek Schmidt. The Medusae Fossae Formation as the single largest source of dust on Mars. Nature Communications, 2018; 9 (1) DOI: 10.1038/s41467-018-05291-5</ref>  Since there are relatively few depositional features in the Medusae Fossae Formation, most of the materials being eroded are probably small enough to be suspended in the atmosphere and transported long distances.<ref>Tanaka, K. L. Dust and ice deposition in the Martian geologic record. Icarus 144, 254–266 (2000).</ref>
 An analysis of data from the 2001 Mars Odyssey Neutron Spectrometer revealed that portions of the Medusae Fossae Formation contain water.<ref>Wilson, J. et al.  2018.  Equatorial locations of water on Mars: Improved resolution maps based on Mars Odyssey Neutron Spectrometer data.  Icarus: 299, 148-160.</ref>

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 |}
-[[File:Collage amazonis.jpg|Features of Amazonis quadrangle, as seen by HiRISE under under HiWish program|600pxr| Features of Amazonis quadrangle]]
+[[File:Collage Amazonis quadrangle 06.jpg|Features of Amazonis quadrangle, as seen by HiRISE under under HiWish program|600pxr| Features of Amazonis quadrangle]]
                                 Scenes of the Amazonis quadrangle

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 |[[Mars Atlas|Atlas]]
 |}
 <gallery widths="400" heights="300">
 File:USGS-Mars-MC-8-AmazonisRegion-mola.png|Amazonis quadrangle elevations

← Older revision		Revision as of 17:40, 11 April 2024
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	Image:Channels From Fissure.JPG\|Channels From Fissure, as seen by HiRISE. The fissure probably started the water flowing to make the channel.		Image:Channels From Fissure.JPG\|Channels From Fissure, as seen by HiRISE. The fissure probably started the water flowing to make the channel.

		+
		+	File:Tilted blocks 82360 1925.jpg\|Tilted blocks It is as if something pushed up from under the ground.
	</gallery>		</gallery>

← Older revision		Revision as of 17:55, 14 January 2024
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">
		+	File:ESP 055285 2030-animationstreaks.gif\|Animation showing changes in streaks on slopes of ridges within the Olympus Mons Aureole. The changes happened in 6 years.

	Esp 036851 1995mesastreaks.jpg\|Dark slope streaks on mesa		Esp 036851 1995mesastreaks.jpg\|Dark slope streaks on mesa

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 1970lvarafts.jpg|Close view of lava rafts from previous images
 Image:Marte Vallis Island.JPG|Streamlined Island in Marte Vallis, as seen by HiRISE.  Island is just to the west of Pettit Crater.  Scale bar is 500 meters long.
-File:Streamlined forms ESP 068107 2080.jpg|Streamline features
 ESP 046478 1975streamlined.jpg|Streamlined feature
 </gallery>

← Older revision		Revision as of 18:00, 23 December 2023
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	[[File:ESP 035480 2015streamlined.jpg\|600pxr\|Streamlined shape showing layers, as seen by HiRISE under [[HiWish program]]]]		[[File:ESP 035480 2015streamlined.jpg\|600pxr\|Streamlined shape showing layers, as seen by HiRISE under [[HiWish program]]]]
−	Streamlined shape showing layers, as seen by HiRISE under [[HiWish program]]	+	Streamlined shape showing layers, as seen by HiRISE under [[HiWish program]]

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 [[File:ESP 043128 2005mesastreaks.jpg|600pxr|Dark slope streaks on layered mesa, as seen by HiRISE under [[HiWish program]]]]
-                              Dark slope streaks on layered mesa, as seen by HiRISE under [[HiWish program]]
+            Dark slope streaks on layered mesa, as seen by HiRISE under [[HiWish program]]
 Dark slope streaks are narrow, avalanche-like features common on dust-covered slopes in the equatorial regions.<ref>Chuang, F.C.; Beyer, R.A.; Bridges, N.T. (2010). Modification of Martian Slope Streaks by Eolian Processes. ''Icarus,'' '''205''' 154–164.</ref> They form in relatively steep sites, such as along escarpments and impact crater walls.<ref>Schorghofer, N.; Aharonson, O.; Khatiwala, S. (2002). Slope Streaks on Mars: Correlations with Surface Properties and the Potential Role of Water. ''Geophys. Res. Lett.,'' '''29'''(23), 2126, </ref> Although first recognized in Viking Orbiter images from the late 1970s,<ref>Morris, E.C. (1982). Aureole Deposits of the Martian Volcano Olympus Mons. ''J. Geophys. Res.,'' '''87'''(B2), 1164–1178.</ref> <ref>Ferguson,H.M.; Lucchitta, B.K. (1984). Dark Streaks on Talus Slopes, Mars in ''Reports of the Planetary Geology Program 1983, NASA Tech. Memo., TM-86246,'' pp. 188–190. https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19840015363_1984015363.pdf.</ref> dark slope streaks were not studied in detail until higher-resolution images from the Mars Global Surveyor (MGS) and Mars Reconnaissance Orbiter (MRO) spacecraft became available in the late 1990s and 2000s.<ref>Sullivan, R. ''et al.'' (2001). Mass Movement Slope Streaks Imaged by the Mars Orbiter Camera. ''J. Geophys. Res.,'' '''106'''(E10), 23,607–23,633.</ref> <ref>Chuang, F.C. ''et al.''  2007.   HiRISE Observations of Slope Streaks on Mars. ''Geophys. Res. Lett.,'' '''34''' L20204, </ref>