Martian features that are signs of water ice - Revision history

Suitupshowup: /* Triangular depressions */ added info and ref about ice in the ground

2025-07-21T15:24:12Z

Triangular depressions: added info and ref about ice in the ground

← Older revision		Revision as of 16:24, 21 July 2025
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	The sites are at latitudes from about 55 to 58 degrees north and south of the equator, suggesting that there is shallow ground ice under roughly a third of the Martian surface.<ref> Steep Slopes on Mars Reveal Structure of Buried Ice. NASA Press Release. 11 January 2018.</ref>		The sites are at latitudes from about 55 to 58 degrees north and south of the equator, suggesting that there is shallow ground ice under roughly a third of the Martian surface.<ref> Steep Slopes on Mars Reveal Structure of Buried Ice. NASA Press Release. 11 January 2018.</ref>

			Several common features on the surface of Mars are common on the Earth where ground ice is present. <ref>https://www-sciencedirect-com.wikipedialibrary.idm.oclc.org/science/article/pii/S0019103525002751</ref> <ref>Soare, R., et al. 2025. “Icy” scarp exposures, “ice-rich” overburdens and ephemeral climate-warming at Mars' mid-latitudes in the very late Amazonian epoch. Icarus. Volume 441, 15 November 2025, 116727</ref>

Suitupshowup: added image of ice under surface in depression

2025-07-12T16:27:12Z

added image of ice under surface in depression

← Older revision		Revision as of 17:27, 12 July 2025
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	ESP 045290 2350triangulardepression.jpg\|Wide view of triangular depressions with ice under thin cover		ESP 045290 2350triangulardepression.jpg\|Wide view of triangular depressions with ice under thin cover
	45290 2350icelayerscloseer.jpg\|Close view of depression, as seen by HiRISE under HiWish program Arrows indicate where there is a very thin, 1-2 meter covering on what is believed to be ice.<ref>https://www.uahirise.org/ESP_071573_2350</ref> <ref>https://www.uahirise.org/ESP_065881_1225</ref>		45290 2350icelayerscloseer.jpg\|Close view of depression, as seen by HiRISE under HiWish program Arrows indicate where there is a very thin, 1-2 meter covering on what is believed to be ice.<ref>https://www.uahirise.org/ESP_071573_2350</ref> <ref>https://www.uahirise.org/ESP_065881_1225</ref>


			File:ESP 065881 1225blueice.jpg\|Ice in triangular depressions, as seen by HiRISE The light blue strip indicates where ice is found in this depression. This ice is just under the surface.
	</gallery>		</gallery>

Suitupshowup: /* Triangular depressions */ added ref about ice in triangular depressions

2025-07-12T16:15:26Z

Triangular depressions: added ref about ice in triangular depressions

← Older revision		Revision as of 17:15, 12 July 2025
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">
	ESP 045290 2350triangulardepression.jpg\|Wide view of triangular depressions with ice under thin cover		ESP 045290 2350triangulardepression.jpg\|Wide view of triangular depressions with ice under thin cover
	45290 2350icelayerscloseer.jpg\|Close view of depression, as seen by HiRISE under HiWish program Arrows indicate where there is a very thin, 1-2 meter covering on what is believed to be ice.<ref>https://www.uahirise.org/ESP_071573_2350</ref>		45290 2350icelayerscloseer.jpg\|Close view of depression, as seen by HiRISE under HiWish program Arrows indicate where there is a very thin, 1-2 meter covering on what is believed to be ice.<ref>https://www.uahirise.org/ESP_071573_2350</ref> <ref>https://www.uahirise.org/ESP_065881_1225</ref>
	</gallery>		</gallery>

Suitupshowup at 21:48, 27 March 2024

2024-03-27T21:48:52Z

← Older revision		Revision as of 22:48, 27 March 2024
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

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

			File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.

	</gallery>		</gallery>


	[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]		[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]

	~~[[File:ESP 025840 2240-3icecrater.gif\|thumb\|200px\|right\|Ice disappearing after being exposed by impact]~~

	Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.		Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.

Suitupshowup at 21:47, 27 March 2024

2024-03-27T21:47:50Z

← Older revision		Revision as of 22:47, 27 March 2024
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

	~~File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.~~

	</gallery>		</gallery>

Suitupshowup at 21:47, 27 March 2024

2024-03-27T21:47:12Z

← Older revision		Revision as of 22:47, 27 March 2024
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	[[File:PIA10741 Possible Ice Below Phoenix.jpg\|thumb\|200px\|right\|View under Phoenix spacecraft Bright regions are probably top of an ice sheet.]]		[[File:PIA10741 Possible Ice Below Phoenix.jpg\|thumb\|200px\|right\|View under Phoenix spacecraft Bright regions are probably top of an ice sheet.]]

	We also observed this process through HiRISE photos of ice first being exposed in new craters and then disappearing.		We also observed this process through HiRISE photos of ice first being exposed in new craters and then disappearing.

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

	File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.		File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.

	</gallery?		</gallery>

	[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]		[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]

Suitupshowup: added image

2024-03-27T21:46:14Z

added image

← Older revision		Revision as of 22:46, 27 March 2024
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	We also observed this process through HiRISE photos of ice first being exposed in new craters and then disappearing.		We also observed this process through HiRISE photos of ice first being exposed in new craters and then disappearing.
			<gallery class="center" widths="380px" heights="360px">

			File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.

			</gallery?
	[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]		[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]

	[[File:ESP 025840 2240-3icecrater.gif\|thumb\|200px\|right\|Ice disappearing after being exposed ~~byu~~ impact]		[[File:ESP 025840 2240-3icecrater.gif\|thumb\|200px\|right\|Ice disappearing after being exposed by impact]

	Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.		Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.

Suitupshowup: added image

2024-03-27T21:43:49Z

added image

← Older revision		Revision as of 22:43, 27 March 2024
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	<gallery class="center" widths="380px" heights="360px">		<gallery class="center" widths="380px" heights="360px">

			File:ESP 025840 2240-3icecrater.gif\|Ice disappering after being exposed by impact.
	45917 2220gulliesmantle.jpg\|Close view that displays the thickness of the mantle		45917 2220gulliesmantle.jpg\|Close view that displays the thickness of the mantle
	46444 2225mantle.jpg\|Mantle, as seen by HiRISE under HiWish program		46444 2225mantle.jpg\|Mantle, as seen by HiRISE under HiWish program

Suitupshowup: added image

2024-03-27T21:41:45Z

added image

← Older revision		Revision as of 22:41, 27 March 2024
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	[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]		[[Image: Iceincraterscomparison.jpg\|thumb\|200px\|left\|Ice in crater Location: 43.286° N and 164.213°E]]

			[[File:ESP 025840 2240-3icecrater.gif\|thumb\|200px\|right\|Ice disappearing after being exposed byu impact]

	Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.		Thanks to the many satellites going around Mars with advanced instruments, we now have a list of features that are signs of easily obtainable underground ice. The shapes of some landscapes are similar to those on the earth that we know contain ice. Radar studies with the SHAllow RADar instrument (SHARD) on board the Mars Reconnaissance Orbiter ( MRO) have found large deposits of ice under relatively thin layers of debris cover for some of these features .<ref> Plaut, J., A. Safaeinili, J. Holt, R. Phillips, J. Head, J., R. Seu, N. Putzig, A. Frigeri. 2009. Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars. Geophys. Res. Lett. 36. doi:10.1029/2008GL036379.</ref> <ref> Holt, J., A. Safaeinili, J. Plaut, J. Head, R. Phillips, R. Seu, S. Kempf, P. Choudhary, D. Young, N. Putzig, D. Biccari, Y. Gim. 2008. Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars. Science 322. doi:10.1126/science.1164246 </ref> The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard MRO has been able to detect spectroscopic signs of water in certain landscapes. The ice caps contain vast resovors of ice, but traveling to the poles is a long way to go for this precious resource. This article will display many landscapes that probably contain easily obtained water ice that are much closer than the poles.

Suitupshowup: /* Ring-Mold Craters */

2023-12-19T00:22:08Z

Ring-Mold Craters

← Older revision		Revision as of 01:22, 19 December 2023
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	Ring-mold craters are a kind of impact crater that looks like the ring molds used in baking.<ref>https://link.springer.com/referenceworkentry/10.1007/978-1-4614-9213-9_318-1</ref> <ref>kress, A., J. Head. 2008. Ring‐mold craters in lineated valley fill and lobate debris aprons on Mars: Evidence for subsurface glacial ice. Geophysical Research Letters Volume 35, Issue 23</ref> They are believed to be caused by an impact into ice.<ref>https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2008GL035501</ref> Ice that is covered by a layer of debris. They are found in parts of Mars that have buried ice. Laboratory experiments confirm that impacts into ice result in a "ring mold shape." They are also bigger than other craters in which an asteroid impacted solid rock. Impacts into ice warm the ice and cause it to flow into the ring mold shape. These craters are common in lobate debris aprons and lineated valley fill.<ref>Kress, A., J. Head. 2008. Ring-mold craters in lineated valley fill and lobate debris aprons on Mars: Evidence for subsurface glacial ice. Geophys.Res. Lett: 35. L23206-8</ref> <ref>Baker, D. et al. 2010. Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars: Evidence for extensive mid-latitude glaciation in the Late Amazonian. Icarus: 207. 186-209</ref> <ref>Kress., A. and J. Head. 2009. Ring-mold craters on lineated valley fill, lobate debris aprons, and concentric crater fill on Mars: Implications for near-surface structure, composition, and age. Lunar Planet. Sci: 40. abstract 1379</ref> They may be an easy way for future colonists of Mars to find water ice because some may contain ice that is relatively pure. Also, since the ring-mold was created during a rebound, ice may have been brought up from below the surface so much less digging or drilling may be required to gather ice.		Ring-mold craters are a kind of impact crater that looks like the ring molds used in baking.<ref>https://link.springer.com/referenceworkentry/10.1007/978-1-4614-9213-9_318-1</ref> <ref>kress, A., J. Head. 2008. Ring‐mold craters in lineated valley fill and lobate debris aprons on Mars: Evidence for subsurface glacial ice. Geophysical Research Letters Volume 35, Issue 23</ref> They are believed to be caused by an impact into ice.<ref>https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2008GL035501</ref> Ice that is covered by a layer of debris. They are found in parts of Mars that have buried ice. Laboratory experiments confirm that impacts into ice result in a "ring mold shape." They are also bigger than other craters in which an asteroid impacted solid rock. Impacts into ice warm the ice and cause it to flow into the ring mold shape. These craters are common in lobate debris aprons and lineated valley fill.<ref>Kress, A., J. Head. 2008. Ring-mold craters in lineated valley fill and lobate debris aprons on Mars: Evidence for subsurface glacial ice. Geophys.Res. Lett: 35. L23206-8</ref> <ref>Baker, D. et al. 2010. Flow patterns of lobate debris aprons and lineated valley fill north of Ismeniae Fossae, Mars: Evidence for extensive mid-latitude glaciation in the Late Amazonian. Icarus: 207. 186-209</ref> <ref>Kress., A. and J. Head. 2009. Ring-mold craters on lineated valley fill, lobate debris aprons, and concentric crater fill on Mars: Implications for near-surface structure, composition, and age. Lunar Planet. Sci: 40. abstract 1379</ref> They may be an easy way for future colonists of Mars to find water ice because some may contain ice that is relatively pure. Also, since the ring-mold was created during a rebound, ice may have been brought up from below the surface so much less digging or drilling may be required to gather ice.

	Note: this is one of the first explanations for ring-mold craters, another has been proposed. The other idea for their formation revolves around the impacting body going through layers with different densities. Also, erosion could have helped shape them. With an extensive analysis of larger areas, it was found the ring mold craters are sometimes formed where there is not as much ice underground.<ref>https://www-sciencedirect-com.wikipedialibrary.idm.oclc.org/science/article/pii/S0019103518301532</ref> <Baker, D. and L. Carter. 2019. Probing supraglacial debris on Mars 2: Crater morphology. Icarus. Volume 319. Pages 264-280</ref>		Note: this is one of the first explanations for ring-mold craters, another has been proposed. The other idea for their formation revolves around the impacting body going through layers with different densities. Also, erosion could have helped shape them. With an extensive analysis of larger areas, it was found the ring mold craters are sometimes formed where there is not as much ice underground.<ref>https://www-sciencedirect-com.wikipedialibrary.idm.oclc.org/science/article/pii/S0019103518301532</ref> <ref>Baker, D. and L. Carter. 2019. Probing supraglacial debris on Mars 2: Crater morphology. Icarus. Volume 319. Pages 264-280</ref>

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