Argyre quadrangle - Revision history

Suitupshowup at 14:16, 24 January 2025

2025-01-24T14:16:32Z

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	\|[[Mars Atlas\|Atlas]]		\|[[Mars Atlas\|Atlas]]
	\|}		\|}

			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.

	<gallery widths="400" heights="300">		<gallery widths="400" heights="300">
	File:USGS-Mars-MC-26-ArgyreRegion-mola.png		File:USGS-Mars-MC-26-ArgyreRegion-mola.png

Suitupshowup: added image

2025-01-01T14:24:53Z

added image

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	File:USGS-Mars-MC-26-ArgyreRegion-mola.png		File:USGS-Mars-MC-26-ArgyreRegion-mola.png
	File:Argyre region on Mars by the Viking 1 orbiter.jpg		File:Argyre region on Mars by the Viking 1 orbiter.jpg
	</gallery>The Argyre quadrangle holds the Argyre basin, a giant impact that occurred 70 million years after the Hellas impact and may have contained a lake in the early history of Mars.		</gallery>

			[[File:Collage Argyre 02.jpg\|Features of Features of Argyre quadrangle, as seen by HiRISE under under HiWish program\|600pxr\| Features of Argyre quadrangle]]

			Scenes of the Argyre quadrangle


			The Argyre quadrangle holds the Argyre basin, a giant impact that occurred 70 million years after the Hellas impact and may have contained a lake in the early history of Mars.

Suitupshowup: /* Martian gullies */

2024-09-06T15:28:10Z

Martian gullies

← Older revision		Revision as of 16:28, 6 September 2024
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	47963 1305gullychannelclose.jpg\|Close view of gully channel Arrow shows small channel within larger channel. Small channel is quite curved in this image.		47963 1305gullychannelclose.jpg\|Close view of gully channel Arrow shows small channel within larger channel. Small channel is quite curved in this image.
	~~File:48364 1410 1kgullies 01.jpg\|Gullies, as seen by HiRISE Picture is about 1 km across.~~
	</gallery>		</gallery>

Suitupshowup: /* Martian gullies */ added images

2024-09-06T15:11:22Z

Martian gullies: added images

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	47963 1305gullychannelclose.jpg\|Close view of gully channel Arrow shows small channel within larger channel. Small channel is quite curved in this image.		47963 1305gullychannelclose.jpg\|Close view of gully channel Arrow shows small channel within larger channel. Small channel is quite curved in this image.
			File:48364 1410 1kgullies 01.jpg\|Gullies, as seen by HiRISE Picture is about 1 km across.
	</gallery>		</gallery>

Suitupshowup: /* Channels */ added image of channels

2024-02-20T14:07:30Z

Channels: added image of channels

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	ESP 047265 1415channel.jpg\|Channel, as seen by HiRISE under HiWish program		ESP 047265 1415channel.jpg\|Channel, as seen by HiRISE under HiWish program
	ESP 048043 1460channel.jpg\|Channel, as seen by HiRISE under HiWish program under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.		ESP 048043 1460channel.jpg\|Channel, as seen by HiRISE under HiWish program under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.
			File:ESP 080141 2170channel 01.jpg\|Wide view of channel as seen by HiRISE under HiWish program. Much erosion is visible in places. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.
			File:ESP 080141 2170channel 02.jpg\|Close view of channel as seen by HiRISE under HiWish program. Much erosion is visible in places. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.

			File:ESP 080141 2170channel 03 Erosion through crater.jpg\|Channel as seen by HiRISE under HiWish program. Arrow indicates where erosion has cut through a crater. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.
	</gallery>		</gallery>

Suitupshowup: added image

2023-11-25T00:14:25Z

added image

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	File:57445 1385dunesclose.jpg\|Close view of dunes Ripples are visible on the dunes.		File:57445 1385dunesclose.jpg\|Close view of dunes Ripples are visible on the dunes.

			File:Dune field in ESP 033272 1400 01.jpg\|Field of dunes as seen by HiRISE
			File:Small group of dunes.jpg\|Close view of group of dunes, as seen by HiRISE under HiWish program
			File:Single dune in Argyre quadrangle.jpg\|Single dune

	</gallery>		</gallery>

Suitupandshowup: /* References */ added external links section

2020-10-15T21:39:25Z

References: added external links section

← Older revision		Revision as of 22:39, 15 October 2020
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	*[[Water]]		*[[Water]]

			==External links==

			*https://planetarynames.wr.usgs.gov/Page/MARS/target For information on names and locations on Mars

			* [https://www.youtube.com/watch?v=NiT02piO40c The Geological History of Water on Mars and Astrobiological Implications (Vic Baker)] (50:10)

			* [https://www.youtube.com/watch?v=RWNXJk0Y01k The Evolution of Water on Mars (Stephen Clifford)] (1:22) (2017)


	==References==		==References==

Suitupandshowup: /* See Also */ added to list

2020-07-07T15:11:58Z

Suitupandshowup at 18:51, 28 March 2020

2020-03-28T18:51:47Z

← Older revision		Revision as of 19:51, 28 March 2020
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">
	~~Happy-face1.jpg\|Galle Crater, also called Happy-Face Crater, as seen by Mars Global Surveyor~~

	ESP 046684 1280molawide.jpg\|Wide view of area around Galle Crater Colors show elevations.		ESP 046684 1280molawide.jpg\|Wide view of area around Galle Crater Colors show elevations.
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	==[[Martian gullies]]==		==[[Martian gullies]]==

	[[File: ESP 040974 1395gullies.jpg\|thumb\|500px\|center\|Wide view of gullies in Arkhangelsky Crater, as seen by HiRISE under[[HiWish program]]]]		[[File: ESP 040974 1395gullies.jpg\|thumb\|500px\|center\|Wide view of gullies in Arkhangelsky Crater, as seen by HiRISE under [[HiWish program]]]]

	Gullies are common in some latitude bands on Mars—usually in midlatitudes. Most Martian gullies are found on the walls of craters or troughs, but Charitum Montes, a group of mountains, has gullies in some ~~areas (See the image below)~~.		Gullies are common in some latitude bands on Mars—usually in midlatitudes. Most Martian gullies are found on the walls of craters or troughs, but Charitum Montes, a group of mountains, has gullies in some locations.

	Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they sometimes are on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. For many years, researchers thought the gullies were made by running water. But after many more observations it was found that gullies are being formed today which cannot happen with liquid water. <ref>Dundas, C., S.		Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they sometimes are on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. For many years, researchers thought the gullies were made by running water. But after many more observations it was found that gullies are being formed today which cannot happen with liquid water. <ref>Dundas, C., S.
	Diniega, and A. McEwen. 2014. LONG-TERM MONITORING OF MARTIAN GULLY ACTIVITY WITH HIRISE. 45th Lunar and Planetary Science Conference. 2204.pdf</ref> <ref>NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm </ref> The weather conditions on present day Mars are such that sufficient liquid water cannot exist to cause gullies to form. Experiments on the Earth showed that gullies can be made with the movement of chunks of dry ice moving down steep slope. <ref>http://spaceref.com/mars/frosty-gullies-on-mars.html</ref> Changes in gullies were seen on Mars when the temperature was just right for such movements of dry ice. <ref>Dundas, C., S. Diniega, A. McEwen. 2015. Long-term monitoring of martian gully formation and evolution with MRO/HiRISE. Icarus: 251, 244–263</ref> <ref> last1 = Raack \| first1 = J. \| display-authors = etal \| year = 2015 \| title = Present-day seasonal gully activity in a south polar pit (Sisyphi Cavi) on Mars\| url = \| journal = Icarus \| volume = 251 \| issue = \| pages = 226–243 \| doi=10.1016/j.icarus.2014.03.040 \| </ref> So, today the scientific community mostly supports the idea that gullies are forming today with dry ice moving down steep slopes. <ref name="NASA-20140710">last=Harrington \|first=J.D. \|last2=Webster \|first2=Guy \|title=RELEASE 14-191 – NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars \|url=http://www.nasa.gov/press/2014/july/nasa-spacecraft-observes-further-evidence-of-dry-ice-gullies-on-mars \|date=July 10, 2014 \|work=NASA</ref> <ref>CNRS. "Gullies on Mars sculpted by dry ice rather than liquid water." ScienceDaily. ScienceDaily, 22 December 2015. www.sciencedaily.com/releases/2015/12/151222082255.htm </ref> <ref>http://www.skyandtelescope.com/astronomy-news/martian-gullies-triggered-by-exploding-dry-ice-122320158</ref> However, some concede that liquid water may have been involved in the past. <ref>Dundas, C., S. Diniega, C. Hansen, S. Byrne, A. McEwen. 2012. Seasonal activity and morphological changes in martian gullies. Icarus, 220. 124–143.</ref>		Diniega, and A. McEwen. 2014. LONG-TERM MONITORING OF MARTIAN GULLY ACTIVITY WITH HIRISE. 45th Lunar and Planetary Science Conference. 2204.pdf</ref> <ref>NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm </ref> The weather conditions on present day Mars are such that sufficient liquid water cannot exist to cause gullies to form. Experiments on the Earth showed that gullies can be made with the movement of chunks of dry ice moving down steep slope. <ref>http://spaceref.com/mars/frosty-gullies-on-mars.html</ref> Changes in gullies were seen on Mars when the temperature was just right for such movements of dry ice. <ref>Dundas, C., S. Diniega, A. McEwen. 2015. Long-term monitoring of martian gully formation and evolution with MRO/HiRISE. Icarus: 251, 244–263</ref> <ref> last1 = Raack \| first1 = J. \| display-authors = etal \| year = 2015 \| title = Present-day seasonal gully activity in a south polar pit (Sisyphi Cavi) on Mars\| url = \| journal = Icarus \| volume = 251 \| issue = \| pages = 226–243 \| doi=10.1016/j.icarus.2014.03.040 \| </ref> So, today the scientific community mostly supports the idea that the gullies that are forming today are doing so with dry ice moving down steep slopes. <ref name="NASA-20140710">last=Harrington \|first=J.D. \|last2=Webster \|first2=Guy \|title=RELEASE 14-191 – NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars \|url=http://www.nasa.gov/press/2014/july/nasa-spacecraft-observes-further-evidence-of-dry-ice-gullies-on-mars \|date=July 10, 2014 \|work=NASA</ref> <ref>CNRS. "Gullies on Mars sculpted by dry ice rather than liquid water." ScienceDaily. ScienceDaily, 22 December 2015. www.sciencedaily.com/releases/2015/12/151222082255.htm </ref> <ref>http://www.skyandtelescope.com/astronomy-news/martian-gullies-triggered-by-exploding-dry-ice-122320158</ref> However, some concede that liquid water may have been involved in the past. <ref>Dundas, C., S. Diniega, C. Hansen, S. Byrne, A. McEwen. 2012. Seasonal activity and morphological changes in martian gullies. Icarus, 220. 124–143.</ref>

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

Suitupandshowup at 17:00, 21 March 2020

2020-03-21T17:00:57Z

← Older revision		Revision as of 18:00, 21 March 2020
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	One of the biggest impact basins on Mars is in the Argyre quadrangle. The Argyre quadrangle covers the area from 30° to 65° south latitude and 0° to 60° west longitude (300 -360 E). It contains [[Galle Crater]], which resembles a smiley face. It contains a region on Mars called [[Argyre Planitia]] and part of another called [[Noachis Terra]]. Noachis is named after Noah in the Bible. This region contains several features that are evidence for ice in the ground. Also, several types of landscapes are very beautiful. These are all discussed and displayed below. Check out the many views from the famous smiley face below.		One of the biggest impact basins on Mars is in the Argyre quadrangle. The Argyre quadrangle covers the area from 30° to 65° south latitude and 0° to 60° west longitude (300 -360 E). It contains Galle Crater, which resembles a smiley face. It contains a region on Mars called Argyre Planitia and part of another called Noachis Terra. Noachis is named after Noah in the Bible. This region contains several features that are evidence for ice in the ground. Also, several types of landscapes are very beautiful. These are all discussed and displayed below. Check out the many views from the famous smiley face below.

	==Name==		==Name==

← Older revision		Revision as of 15:07, 20 February 2024
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	ESP 047265 1415channel.jpg\|Channel, as seen by HiRISE under HiWish program		ESP 047265 1415channel.jpg\|Channel, as seen by HiRISE under HiWish program
	ESP 048043 1460channel.jpg\|Channel, as seen by HiRISE under HiWish program under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.		ESP 048043 1460channel.jpg\|Channel, as seen by HiRISE under HiWish program under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.
			File:ESP 080141 2170channel 01.jpg\|Wide view of channel as seen by HiRISE under HiWish program. Much erosion is visible in places. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.
			File:ESP 080141 2170channel 02.jpg\|Close view of channel as seen by HiRISE under HiWish program. Much erosion is visible in places. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.

			File:ESP 080141 2170channel 03 Erosion through crater.jpg\|Channel as seen by HiRISE under HiWish program. Arrow indicates where erosion has cut through a crater. Since July 23, 2023, HiRISE observations have lacked data from the RED4 CCD due to a hardware issue, creating a gap in the middle of image products.
	</gallery>		</gallery>

← Older revision		Revision as of 16:11, 7 July 2020
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	*[[Dust devils]]		*[[Dust devils]]
			*[[Geography of Mars]]
	*[[High Resolution Imaging Science Experiment (HiRISE)]]		*[[High Resolution Imaging Science Experiment (HiRISE)]]
	*[[HiWish program]]		*[[HiWish program]]