Eridania quadrangle - Revision history

Suitupshowup: /* Craters */

2025-01-22T16:45:16Z

Craters

Suitupshowup: /* Craters */

2025-01-22T16:43:37Z

Craters

Suitupshowup: /* Craters */ added new inf and ref

2025-01-22T16:40:15Z

Craters: added new inf and ref

Suitupshowup at 02:30, 22 January 2025

2025-01-22T02:30:12Z

Suitupshowup: added image

2025-01-01T14:58:58Z

added image

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

2024-09-06T15:31:46Z

Other features in Eridania quadrangle: added image

Suitupshowup: /* Martian gullies */ added images

2024-09-06T15:29:32Z

Martian gullies: added images

Suitupshowup: added new info and ref

2024-04-17T13:09:12Z

added new info and ref

Suitupshowup: /* Martian gullies */

2023-12-24T00:56:47Z

Martian gullies

Suitupshowup: /* Martian gullies */

2023-12-24T00:56:23Z

Martian gullies

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 Much material is thrown out around the crater; the material is called ejecta.  Some of the material comes from deep underground; therefore, samples gathered from that place can tell us about minerals under the surface. In the end, a  bowl-shaped cavity is made.  Also, a rim is made.  As time passes, the ejecta gets covered with dust and the cavity gets less deep.
-Most impact craters are roughly circular due to the explosion of energy outwards from the impact point.  <ref>https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock</ref> As craters get larger (greater than 10&nbsp;km in diameter) they usually have a central peak.<ref>{{Cite web|url=http://www.lpi.usra.edu/publications/slidesets/stones/|title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|access-date=7 March 2011|year=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref>
+Most impact craters are roughly circular due to the explosion of energy outwards from the impact point.  <ref>https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock</ref> As craters get larger (greater than 10&nbsp;km in diameter) they usually have a central peak.<ref>{{|url=http://www.lpi.usra.edu/publications/slidesets/stones/|title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|access-date=7 March 2011|year=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref>
 <gallery class="center"  widths="380px" heights="360px">

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 Much material is thrown out around the crater; the material is called ejecta.  Some of the material comes from deep underground; therefore, samples gathered from that place can tell us about minerals under the surface. In the end, a  bowl-shaped cavity is made.  Also, a rim is made.  As time passes, the ejecta gets covered with dust and the cavity gets less deep.
-Most impact craters are roughly circular due to the explosion of energy outwards from the impact point.  <ref>https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock</ref> As craters get larger (greater than 10&nbsp;km in diameter) they usually have a central peak.<ref>{{Cite web|url=http://www.lpi.usra.edu/publications/slidesets/stones/|title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{cite book|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|access-date=7 March 2011|year=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref>
+Most impact craters are roughly circular due to the explosion of energy outwards from the impact point.  <ref>https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock</ref> As craters get larger (greater than 10&nbsp;km in diameter) they usually have a central peak.<ref>{{Cite web|url=http://www.lpi.usra.edu/publications/slidesets/stones/|title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|access-date=7 March 2011|year=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref>
 <gallery class="center"  widths="380px" heights="360px">
 Image:28415facewide.jpg|Crater floor with the shape of an odd face The box indicates where the next picture is located.

← Older revision		Revision as of 16:40, 22 January 2025
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	==Craters==		==Craters==
		+
		+	Impact craters are created when a fast moving body strikes the surface. The force of the impact pushes the ground under the impact point. A shock wave then travels outwards, fracturing and ejecting rock and debris.
		+
		+	Much material is thrown out around the crater; the material is called ejecta. Some of the material comes from deep underground; therefore, samples gathered from that place can tell us about minerals under the surface. In the end, a bowl-shaped cavity is made. Also, a rim is made. As time passes, the ejecta gets covered with dust and the cavity gets less deep.
		+	Most impact craters are roughly circular due to the explosion of energy outwards from the impact point. <ref>https://askanearthspacescientist.asu.edu/top-question/how-craters-form#:~:text=For%20example%2C%20rocks%20collected%20from,energy%20to%20the%20surrounding%20rock</ref> As craters get larger (greater than 10 km in diameter) they usually have a central peak.<ref>{{Cite web\|url=http://www.lpi.usra.edu/publications/slidesets/stones/\|title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}</ref> The peak is caused by a rebound of the crater floor following the impact.<ref name="Kieffer1992">{{cite book\|author=Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|access-date=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7}}</ref>

	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

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 In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood.
-The Eridania quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey. The Eridania quadrangle is also referred to as MC-29 (Mars Chart-29).<ref>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.</ref>  The Eridania quadrangle lies between 30° and 65° south latitude and 180° and 240° west longitude (180-120 E).  Most of the classic region named Terra Cimmeria is found within this quadrangle.  It is named after a region on the Po River, Italy.   The name was approved by the IAUP in 1958.<ref>https://planetarynames.wr.usgs.gov/Feature/1826</ref
+The Eridania quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey. The Eridania quadrangle is also referred to as MC-29 (Mars Chart-29).<ref>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.</ref>  The Eridania quadrangle lies between 30° and 65° south latitude and 180° and 240° west longitude (180-120 E).  Most of the classic region named Terra Cimmeria is found within this quadrangle.  It is named after a region on the Po River, Italy.   The name was approved by the IAUP in 1958.<ref>https://planetarynames.wr.usgs.gov/Feature/1826</ref>
 Part of the Electris deposits, a 100–200 meters thick, light-toned deposit covers the Eridania quadrangle.<ref>Grant, J. and P. Schultz.  1990.  Gradational epochs on Mars: Evidence from west-northwest of Isidis Basin and Electric.  Icarus: 84. 166-195.</ref>

← Older revision		Revision as of 14:58, 1 January 2025
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	File:PIA00189-MC-29-EridaniaRegion-19980605.jpg		File:PIA00189-MC-29-EridaniaRegion-19980605.jpg
	</gallery>		</gallery>
		+
		+
		+	[[File:Collage Eridania 05.jpg\|Features of Eridania quadrangle, as seen by HiRISE under under HiWish program\|600pxr\| Features of Eridania quadrangle]]
		+
		+	Scenes of the Eridania quadrangle

← Older revision		Revision as of 15:31, 6 September 2024
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	File:ESP 055104 1385pyramid.jpg\|Layered feature in a crater		File:ESP 055104 1385pyramid.jpg\|Layered feature in a crater
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		+	File:Layers on crater wall 48364 1410.jpg\|Layers in crater wall, as seen by HiRISE under HiWish program. Differeht colors mean different minerals.
	</gallery>		</gallery>

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 ESP 048364 1410gullieslayers.jpg|Crater with gullies
+File:48364 1410 1kgullies 01.jpg|Gullies, as seen by HiRISE  Picture is about 1 km across.
 </gallery>

← Older revision		Revision as of 00:56, 24 December 2023
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	[[File:ESP 055063 1410gullywidecropped.jpg\|600pxr\|Labeled gully, as seen by HiRISE under HiWish program]]		[[File:ESP 055063 1410gullywidecropped.jpg\|600pxr\|Labeled gully, as seen by HiRISE under HiWish program]]

−	Labeled gully, as seen by HiRISE under HiWish program	+	Labeled gully, as seen by HiRISE under HiWish program