Mare Acidalium quadrangle - Revision history

Suitupshowup: /* Mud volcanoes */ added section about crater lakes

2026-04-06T17:13:29Z

Mud volcanoes: added section about crater lakes

Suitupshowup: /* Craters */

2026-04-06T17:09:02Z

Craters

Suitupshowup at 16:00, 24 January 2025

2025-01-24T16:00:28Z

Suitupshowup: /* Craters */

2025-01-22T16:19:54Z

Craters

Suitupshowup: /* Craters */

2025-01-22T15:40:07Z

Craters

Suitupshowup: /* Craters */

2025-01-22T15:38:38Z

Craters

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

2025-01-22T15:36:42Z

Craters: added new info and ref

Suitupshowup: /* Mud volcanoes */ removed image

2025-01-22T02:24:24Z

Mud volcanoes: removed image

Suitupshowup: added image

2024-11-23T16:21:11Z

added image

Suitupshowup: /* Mud volcanoes */

2024-10-07T19:03:46Z

Mud volcanoes

← Older revision		Revision as of 17:13, 6 April 2026
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	</gallery>		</gallery>
		+
		+	==Crater Lakes==
		+
		+	Many craters on Mars probably became lakes. <ref> Fassett C. I. and Head J. W. 2008. Icarus. 195 61</ref> <ref> Goudge T. A., Aureli K. L., Head J. W., Fassett C. I. and Mustard J. F. 2015 Icarus. 260 346</ref> There could have been several sources for the water. Like:
		+	(1) Runoff and River Inlets: Many craters show evidence of channels eroded into their rims, indicating that water flowed across the landscape and broke through the crater walls. Dense, branching valley networks across the southern highlands suggest that ancient rain or snowmelt carved channels that eventually breached crater rims. <ref>Bamber, E. R., Goudge, T. A., Fassett, C. I., Osinski, G. R., & Stucky de Quay, G. (2022). Paleolake inlet valley formation: Factors controlling which craters breached on early Mars. Geophysical Research Letters, 49, e2022GL101097. https://doi.org/10.1029/2022GL101097</ref>
		+	(2) Glacial Melting: Researchers have found evidence that some lakes were fed by runoff from glaciers. In this scenario, glaciers occupying the area, or sitting on the crater walls, melted and transported water to the center of the crater.
		+	(3) Groundwater Sapping: In some cases, water may have broken through the ground surface, known as groundwater sapping, feeding the lake from below or through the crater walls.<ref> Goudge T. A., Aureli K. L., Head J. W., Fassett C. I. and Mustard J. F. 2015 Icarus. 260 346
		+	</ref> <ref>Salese F., Pondrelli M., Neeseman A., Schmidt G. and Ori G. G. 2019. JGRE. Vol. 124. P. 374</ref> Some craters, lack large surface inflow channels. Instead, they feature layered rocks containing carbonate and clay minerals, suggesting that groundwater from underground aquifers came up through fractures in the crater floor.<ref>https://www.jpl.nasa.gov/news/martian-crater-may-once-have-held-groundwater-fed-lake/</ref>
		+
		+	Once water accumulated in a crater, it behaved in ways similar to terrestrial lakes.
		+	Delta Formation: As water entered the crater via an inlet channel, it slowed down and dropped its sediment load, creating fan-shaped structures known as deltas. The Perseverance Rover has documented these, along with sloping layers known as foreset beds, which are characteristic of deltas building into a lake. At times, water input was so significant that the lakes filled to the brim and overflowed the crater rim, creating outlet canyons and changing the surrounding landscape.
		+
		+	<gallery class="center" widths="380px" heights="360px">
		+	File:ESP 078227 2195lake.jpg\|Channels that filled crater to make a crater lake, as seen by HiRISE under HiWish program.
		+
		+	</gallery>
		+
		+	Martian crater lakes may have lasted from a million years down to just a century.<ref>https://www.nhm.ac.uk/discover/news/2022/september/ancient-crater-lakes-mars-could-have-hosted-life.html</ref>
		+
		+
		+
		+
		+
		+

	==Mud volcanoes==		==Mud volcanoes==

@@ Line 97: / Line 97: @@
 Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat.  If one measures the diameter of a crater, the original depth can be estimated with various ratios.  Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al.  2002.  Global geometric properities of martian impact craters.  Lunar Planet Sci. 33.  Abstract @1255.</ref>  Some of these flat floored craters display numberous concentric lines--they are called concentric crater fill craters.  Craters like these may be used by future colonists for water.  Before we land, we will have a map of where these water sources are.  Eventually, we will probably develop robotic machines to extract the water.
 <gallery class="center"  widths="380px" heights="360px">
@@ Line 104: / Line 103: @@
 Image:Exhumedburied Craterin Coprates.jpg|Exhumed Crater in Mare Acidalium, as seen by [[Mars Global Surveyor]]  This crater was buried and now it is being uncovered.
 Image:ESP 026594 1470closecraters.jpg|Craters that formed at the same time.   If the craters were formed at different times, they would have wiped away parts of the others. These craters may been made when an asteroid broke up in the atmosphere. Picture was taken by HiRISE, under HiWish program.  Image located in Terra Cimmeria.

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 |[[Mars Atlas|Atlas]]
 |}
 <gallery widths="400" heights="300">
 File:USGS-Mars-MC-4-MareAcidaliumRegion-mola.png
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 The quadrangle contains many interesting features, including gullies and possible shorelines of an ancient northern ocean.  Some areas are densely layered.  The boundary between the southern highlands and the northern lowlands lies in Mare Acidalium.<ref>http://hirise.lpl.arizona.edu/PSP_010354_2165</ref>   The Cydonia Region includes the Face on Mars (located near 40.8 degrees north and 9.6 degrees west).  When Mars Global Surveyor examined it with high resolution, the face turned out to just be an eroded mesa.<ref>http://mars.jpl.nasa.gov/mgs/msss/camera/images/moc_5_24_01/face/index.html</ref>  Mare Acidalium contains the Kasei Valles system of canyons.  This huge system is 300 miles wide in some places—Earth's Grand Canyon is only 18 miles wide.<ref>http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_001640_2125</ref>
-[[File:Collage marea cidalium.jpg|Typical features of Mare Acidalium quadrangle, as seen by HiRISE under under HiWish program|600pxr| Typical features of Mare Acidalium quadrangle]]
+[[File:Collage mare acidalium02.jpg|Typical features of Mare Acidalium quadrangle, as seen by HiRISE under under HiWish program|600pxr| Typical features of Mare Acidalium quadrangle]]
                                 Typical features of Mare Acidalium quadrangle

← Older revision		Revision as of 16:19, 22 January 2025
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	Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.		Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.

−	Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.</ref> Some of these flat floored craters display ~~numberouc~~ concentric lines--they are called concentric crater fill craters. Craters like these may be used by future colonists for water. Before we land, we will have a map of where these water sources are. Eventually, we will probably develop robotic machines to extract the water.	+	Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.</ref> Some of these flat floored craters display numberous concentric lines--they are called concentric crater fill craters. Craters like these may be used by future colonists for water. Before we land, we will have a map of where these water sources are. Eventually, we will probably develop robotic machines to extract the water.

@@ Line 108: / Line 108: @@
 Image:ESP 027538 2265.jpg|Crater wall covered with a smooth mantle
-ESP 052749 2285pits.jpg|Crater with pits on floor, as seen by HiRISE under [[HiWish program]]
+ESP 052749 2285pits.jpg|Concentric crater fill crater with pits on floor, as seen by HiRISE under [[HiWish program]]
 </gallery>

← Older revision		Revision as of 15:38, 22 January 2025
Line 95:		Line 95:
	Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.		Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.

−	Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.</ref> Some of these flat floored craters display numberouc concentric lines--they are called concentric crater fill craters. Craters like these may be used by future colonists for water. Before we land, we will have a map of where these water sources are. Eventually, we will probably develop ~~robitic~~ machines to extract the water.	+	Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.</ref> Some of these flat floored craters display numberouc concentric lines--they are called concentric crater fill craters. Craters like these may be used by future colonists for water. Before we land, we will have a map of where these water sources are. Eventually, we will probably develop robotic machines to extract the water.

← Older revision		Revision as of 15:36, 22 January 2025
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	Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.		Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.<ref>Hugh H. Kieffer\|title=Mars\|url=https://books.google.com/books?id=NoDvAAAAMAAJ\|accessdate=7 March 2011\|year=1992\|publisher=University of Arizona Press\|isbn=978-0-8165-1257-7 </ref> Sometimes craters 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.
		+
		+	Craters usually get a bowl shape when first formed, but with age, debris and ice fall in it and make it more flat. If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.<ref>Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.</ref> Some of these flat floored craters display numberouc concentric lines--they are called concentric crater fill craters. Craters like these may be used by future colonists for water. Before we land, we will have a map of where these water sources are. Eventually, we will probably develop robitic machines to extract the water.
		+

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

← Older revision		Revision as of 02:24, 22 January 2025
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	ESP 040775 2235cones.jpg\|Large field of cones that may be mud volcanoes		ESP 040775 2235cones.jpg\|Large field of cones that may be mud volcanoes
−	~~File:Mottled terrain ESP 080653 2255.jpg\|Mottled terrain that consists of mud volcanoes~~
	040775 2235conesclose.jpg\|Close-up of possible mud volcanoes Note: this is an enlargement of the previous image.		040775 2235conesclose.jpg\|Close-up of possible mud volcanoes Note: this is an enlargement of the previous image.

← Older revision		Revision as of 16:21, 23 November 2024
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	The quadrangle contains many interesting features, including gullies and possible shorelines of an ancient northern ocean. Some areas are densely layered. The boundary between the southern highlands and the northern lowlands lies in Mare Acidalium.<ref>http://hirise.lpl.arizona.edu/PSP_010354_2165</ref> The Cydonia Region includes the Face on Mars (located near 40.8 degrees north and 9.6 degrees west). When Mars Global Surveyor examined it with high resolution, the face turned out to just be an eroded mesa.<ref>http://mars.jpl.nasa.gov/mgs/msss/camera/images/moc_5_24_01/face/index.html</ref> Mare Acidalium contains the Kasei Valles system of canyons. This huge system is 300 miles wide in some places—Earth's Grand Canyon is only 18 miles wide.<ref>http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_001640_2125</ref>		The quadrangle contains many interesting features, including gullies and possible shorelines of an ancient northern ocean. Some areas are densely layered. The boundary between the southern highlands and the northern lowlands lies in Mare Acidalium.<ref>http://hirise.lpl.arizona.edu/PSP_010354_2165</ref> The Cydonia Region includes the Face on Mars (located near 40.8 degrees north and 9.6 degrees west). When Mars Global Surveyor examined it with high resolution, the face turned out to just be an eroded mesa.<ref>http://mars.jpl.nasa.gov/mgs/msss/camera/images/moc_5_24_01/face/index.html</ref> Mare Acidalium contains the Kasei Valles system of canyons. This huge system is 300 miles wide in some places—Earth's Grand Canyon is only 18 miles wide.<ref>http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_001640_2125</ref>
		+
		+	[[File:Collage marea cidalium.jpg\|Typical features of Mare Acidalium quadrangle, as seen by HiRISE under under HiWish program\|600pxr\| Typical features of Mare Acidalium quadrangle]]
		+
		+	Typical features of Mare Acidalium quadrangle
		+

	==Origin of name==		==Origin of name==

@@ Line 133: / Line 133: @@
 ESP 052050 2200mudvolcanoes.jpg|Wide view of field of mud volcanoes
-File:84807 2225conecolor 01.jpg|Close view of mud volcanoe, as seen by HiRISE.  Picture is about 1 km across.  This mud volcano has a different color than the surroundings because it consists of material brought up from depth.  These structures may be useful to explore for reamins of past life since they contain samples that would have been protected from the strong radiation at the surface.
+File:84807 2225conecolor 01.jpg|Close view of mud volcano, as seen by HiRISE.  Picture is about 1 km across.  This mud volcano has a different color than the surroundings because it consists of material brought up from depth.  These structures may be useful to explore for reamins of past life since they contain samples that would have been protected from the strong radiation at the surface.
 </gallery>