What Mars Actually Looks Like! - Revision history

Suitupshowup: /* Craters */ added image

2025-12-01T13:28:52Z

Craters: added image

← Older revision		Revision as of 14:28, 1 December 2025
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	Most of the surface of Mars is over a billion years old. Because Mars has not had active plate tectonics for a very long time (if it ever had active plate tectonics), impact craters stay for a long time. So, impact craters are a major surface feature. There is a rich variety of craters on the planet.<ref>https://en.wikipedia.org/wiki/List_of_craters_on_Mars</ref> <ref>Carr, M.H. (2006) The surface of Mars; Cambridge University Press: Cambridge, UK</ref> We have found that Mars is hit by 200 impacts/year.<ref>https://www.space.com/21198-mars-asteroid-strikes-common.html</ref> <ref>https://www.sciencedirect.com/science/article/abs/pii/S0019103513001693?via%3Dihub</ref> <ref>Daubar, I., et al. 2013. The current martian cratering rate. Icarus. Volume 225. 506-516. </ref>		Most of the surface of Mars is over a billion years old. Because Mars has not had active plate tectonics for a very long time (if it ever had active plate tectonics), impact craters stay for a long time. So, impact craters are a major surface feature. There is a rich variety of craters on the planet.<ref>https://en.wikipedia.org/wiki/List_of_craters_on_Mars</ref> <ref>Carr, M.H. (2006) The surface of Mars; Cambridge University Press: Cambridge, UK</ref> We have found that Mars is hit by 200 impacts/year.<ref>https://www.space.com/21198-mars-asteroid-strikes-common.html</ref> <ref>https://www.sciencedirect.com/science/article/abs/pii/S0019103513001693?via%3Dihub</ref> <ref>Daubar, I., et al. 2013. The current martian cratering rate. Icarus. Volume 225. 506-516. </ref>


			[[File:Features in and around Martian craters.jpg\|600pxr\|Features in and around Martian craters]]

			Features in and around Martian craters

	[[File:ESP 059649 1695craterpretty.jpg \|Young crater with bright ejecta in the Phoenicis Lacus quadrangle as seen by HiRISE under HiWish program The impact reached down to a layer that is light-toned. That light-toned material was then deposited on a dark surface.		[[File:ESP 059649 1695craterpretty.jpg \|Young crater with bright ejecta in the Phoenicis Lacus quadrangle as seen by HiRISE under HiWish program The impact reached down to a layer that is light-toned. That light-toned material was then deposited on a dark surface.

Suitupshowup: /* Dust devil tracks */ added new info and ref

2025-10-15T12:54:17Z

Dust devil tracks: added new info and ref

← Older revision		Revision as of 13:54, 15 October 2025
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	<ref>https://www.science.org/doi/10.1126/sciadv.abn3783</ref> <ref> Newman, C., et al. 2022. The dynamic atmospheric and aeolian environment of Jezero crater, Mars. Science Advances. Vol. 8. Number 21</ref> Perseverance Rover recorded a tall dust devil in the distance on Aug. 30, 2023.		<ref>https://www.science.org/doi/10.1126/sciadv.abn3783</ref> <ref> Newman, C., et al. 2022. The dynamic atmospheric and aeolian environment of Jezero crater, Mars. Science Advances. Vol. 8. Number 21</ref> Perseverance Rover recorded a tall dust devil in the distance on Aug. 30, 2023.
	Scientists calculated that the dust devil was about 2.5 miles (4 kilometers) away and was moving east to west at about 12 mph (19 kph). Its width was about 200 feet (60 meters). Even though only the bottom 387 feet (118 meters) of the devil was visible in the camera frame, scientists estimated its total height at about 1.2 miles (2 kilometers) using the dust devil's shadow.<ref>https://www.jpl.nasa.gov/images/pia26074-martian-whirlwind-takes-the-thorofare</ref>		Scientists calculated that the dust devil was about 2.5 miles (4 kilometers) away and was moving east to west at about 12 mph (19 kph). Its width was about 200 feet (60 meters). Even though only the bottom 387 feet (118 meters) of the devil was visible in the camera frame, scientists estimated its total height at about 1.2 miles (2 kilometers) using the dust devil's shadow.<ref>https://www.jpl.nasa.gov/images/pia26074-martian-whirlwind-takes-the-thorofare</ref>

			Researchers V. Bickel and others, studied over a thousand dust devils and published their results in 2025. The study found that the diameters of dust devils range from an estimated ~18 to ~578 m, with a average diameter of 82 m.<ref> https://www.science.org/doi/10.1126/sciadv.adw5170?adobe_mc=MCMID%3D68227027333727904592434133527388632768%7CMCORGID%3D242B6472541199F70A4C98A6%2540AdobeOrg%7CTS%3D1759927070&adobe_mc=MCMID%3D68227027333727904592434133527388632768%7CMCORGID%3D242B6472541199F70A4C98A6%2540AdobeOrg%7CTS%3D1759927073&adobe_mc=MCMID%3D68227027333727904592434133527388632768%7CMCORGID%3D242B6472541199F70A4C98A6%2540AdobeOrg%7CTS%3D1759927544%27</ref> <ref>Valentin T. Bickel et al. ,Dust devil migration patterns reveal strong near-surface winds across Mars.Sci. Adv.11,eadw5170(2025).DOI:10.1126/sciadv.adw5170</ref>

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

Suitupshowup: /* Glaciers */

2025-09-01T21:48:58Z

Glaciers

← Older revision		Revision as of 22:48, 1 September 2025
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	There are large areas on Mars that contain what is thought to be ice moving under a cover of debris. A few meters of debris can preserve ice for long periods of time.<ref>Head, J. W.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change". Earth and Planetary Science Letters. 241 (3): 663–671.</ref>		There are large areas on Mars that contain what is thought to be ice moving under a cover of debris. A few meters of debris can preserve ice for long periods of time.<ref>Head, J. W.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change". Earth and Planetary Science Letters. 241 (3): 663–671.</ref>

	In a paper published in Icarus, analysis of [[SHARAD]] data led researchers to conclude that glaciers are over 80% pure ice. The authors examined five different sites from around the planet and all showed high levels of pure water ice. <ref> Yuval Steinberg et al, "Physical properties of subsurface water ice deposits in Mars's Mid-Latitudes from the shallow radar.", Icarus (2025)</ref> <ref> https://www.space.com/astronomy/mars/good-news-for-mars-settlers-red-planet-glaciers-are-mostly-pure-water-ice-study-suggests</ref> <ref>https://www.youtube.com/watch?v=nzh2sirXfD8</ref>		In a paper published in Icarus, analysis of SHARAD data led researchers to conclude that glaciers are over 80% pure ice. The authors examined five different sites from around the planet and all showed high levels of pure water ice. <ref> Yuval Steinberg et al, "Physical properties of subsurface water ice deposits in Mars's Mid-Latitudes from the shallow radar.", Icarus (2025)</ref> <ref> https://www.space.com/astronomy/mars/good-news-for-mars-settlers-red-planet-glaciers-are-mostly-pure-water-ice-study-suggests</ref> <ref>https://www.youtube.com/watch?v=nzh2sirXfD8</ref>

	Because of the high purity of the ice content that was found, the authors argued that the formation of glaciers happened by atmospheric precipitation or direct condensation. After glaciers were formed there was a time when enhanced sublimation formed a lag layer or promoted the accumulation of dry debris atop the water ice glacier. Those dry debris would then insulate the underlying ice from going away.<ref> Steinberg, Y. et al. 2025. Physical properties of subsurface water ice deposits in Mars’s Mid-Latitudes from the shallow radar. Icarus. vol. 441 116716</ref>		Because of the high purity of the ice content that was found, the authors argued that the formation of glaciers happened by atmospheric precipitation or direct condensation. After glaciers were formed there was a time when enhanced sublimation formed a lag layer or promoted the accumulation of dry debris atop the water ice glacier. Those dry debris would then insulate the underlying ice from going away.<ref> Steinberg, Y. et al. 2025. Physical properties of subsurface water ice deposits in Mars’s Mid-Latitudes from the shallow radar. Icarus. vol. 441 116716</ref>

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

2025-09-01T21:48:20Z

Glaciers: added new info and ref

← Older revision		Revision as of 22:48, 1 September 2025
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	There are large areas on Mars that contain what is thought to be ice moving under a cover of debris. A few meters of debris can preserve ice for long periods of time.<ref>Head, J. W.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change". Earth and Planetary Science Letters. 241 (3): 663–671.</ref>		There are large areas on Mars that contain what is thought to be ice moving under a cover of debris. A few meters of debris can preserve ice for long periods of time.<ref>Head, J. W.; et al. (2006). "Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change". Earth and Planetary Science Letters. 241 (3): 663–671.</ref>

			In a paper published in Icarus, analysis of [[SHARAD]] data led researchers to conclude that glaciers are over 80% pure ice. The authors examined five different sites from around the planet and all showed high levels of pure water ice. <ref> Yuval Steinberg et al, "Physical properties of subsurface water ice deposits in Mars's Mid-Latitudes from the shallow radar.", Icarus (2025)</ref> <ref> https://www.space.com/astronomy/mars/good-news-for-mars-settlers-red-planet-glaciers-are-mostly-pure-water-ice-study-suggests</ref> <ref>https://www.youtube.com/watch?v=nzh2sirXfD8</ref>

			Because of the high purity of the ice content that was found, the authors argued that the formation of glaciers happened by atmospheric precipitation or direct condensation. After glaciers were formed there was a time when enhanced sublimation formed a lag layer or promoted the accumulation of dry debris atop the water ice glacier. Those dry debris would then insulate the underlying ice from going away.<ref> Steinberg, Y. et al. 2025. Physical properties of subsurface water ice deposits in Mars’s Mid-Latitudes from the shallow radar. Icarus. vol. 441 116716</ref>

	Several types of landforms have been identified as probably dirt and rock debris covering huge deposits of ice.<ref>Head, J. and D. Marchant. 2006. Evidence for global-scale northern mid-latitude glaciation in the Amazonian period of Mars: Debris-covered glacial and valley glacial deposits in the 30 - 50 N latitude band. Lunar. Planet. Sci. 37. Abstract 1127</ref> <ref>Head, J. and D. Marchant. 2006. Modifications of the walls of a Noachian crater in Northern Arabia Terra (24 E, 39 N) during northern mid-latitude Amazonian glacial epochs on Mars: Nature and evolution of Lobate Debris Aprons and their relationships to lineated valley fill and glacial systems. Lunar. Planet. Sci. 37. Abstract 1128</ref> <ref>Head, J., et al. 2006. Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for the late Amazonian obliquity-driven climate change. Earth Planet. Sci. Lett. 241. 663-671</ref> <ref>Head, J., et al. 2006. Modification if the dichotomy boundary on Mars by Amazonian mid-latitude regional glaciation. Geophys. Res Lett. 33</ref> Concentric crater fill (CCF) contains dozens to hundreds of concentric ridges that are caused by the movements of sometimes hundreds of meter thick accumulations of ice in craters.<ref>Garvin, J. et al. 2002. Lunar Planet. Sci: 33. Abstract # 1255.</ref> <ref>http://photojournal.jpl.nasa.gov/catalog/PIA09662</ref> Lineated valley fill (LVF) are lines of ridges in valleys.<ref>Carr, M. 2006. The Surface of Mars. Cambridge University Press. ISBN\|978-0-521-87201-0</ref> <ref>Squyres, S. 1978. Martian fretted terrain: Flow of erosional debris. Icarus: 34. 600-613.</ref> <ref>Levy, J. et al. 2007. Lineated valley fill and lobate debris apron stratigraphy in Nilosyrtis Mensae, Mars: Evidence for phases of glacial modification of the dichotomy boundary. J. Geophys. Res. 112</ref> These lines may have developed as other glaciers moved down valleys. Some of these glaciers seem to come from material sitting around mesas and buttes.<ref>Baker, D., et al. 2009. 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> Lobate debris aprons (LDA) is the name given to these glaciers. All of these features that are believed to contain large amounts of ice are found in the mid-latitudes in both the Northern and Southern hemispheres.<ref>Marchant, D. and J. Head. 2007. Antarctic dry valleys: Microclimate zonation, variable geomorphic processes, and implications for assessing climatic change on Mars. Icarus: 192.187-222</ref> <ref>Dickson, J., et al. 2008. Late Amazonian glaciation at the dichotomy boundary on Mars: Evidence for glacial thickness maxima and multiple glacial phases. Geology: 36 (5) 411-415</ref> <ref>Kress, A., et al. 2006. The nature of the transition from lobate debris aprons to lineated valley fill: Mamers Valles, Northern Arabia Terra-Deuteronilus Mensae region on Mars. Lunar. Planet. Sci. 37. Abstract 1323</ref>		Several types of landforms have been identified as probably dirt and rock debris covering huge deposits of ice.<ref>Head, J. and D. Marchant. 2006. Evidence for global-scale northern mid-latitude glaciation in the Amazonian period of Mars: Debris-covered glacial and valley glacial deposits in the 30 - 50 N latitude band. Lunar. Planet. Sci. 37. Abstract 1127</ref> <ref>Head, J. and D. Marchant. 2006. Modifications of the walls of a Noachian crater in Northern Arabia Terra (24 E, 39 N) during northern mid-latitude Amazonian glacial epochs on Mars: Nature and evolution of Lobate Debris Aprons and their relationships to lineated valley fill and glacial systems. Lunar. Planet. Sci. 37. Abstract 1128</ref> <ref>Head, J., et al. 2006. Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for the late Amazonian obliquity-driven climate change. Earth Planet. Sci. Lett. 241. 663-671</ref> <ref>Head, J., et al. 2006. Modification if the dichotomy boundary on Mars by Amazonian mid-latitude regional glaciation. Geophys. Res Lett. 33</ref> Concentric crater fill (CCF) contains dozens to hundreds of concentric ridges that are caused by the movements of sometimes hundreds of meter thick accumulations of ice in craters.<ref>Garvin, J. et al. 2002. Lunar Planet. Sci: 33. Abstract # 1255.</ref> <ref>http://photojournal.jpl.nasa.gov/catalog/PIA09662</ref> Lineated valley fill (LVF) are lines of ridges in valleys.<ref>Carr, M. 2006. The Surface of Mars. Cambridge University Press. ISBN\|978-0-521-87201-0</ref> <ref>Squyres, S. 1978. Martian fretted terrain: Flow of erosional debris. Icarus: 34. 600-613.</ref> <ref>Levy, J. et al. 2007. Lineated valley fill and lobate debris apron stratigraphy in Nilosyrtis Mensae, Mars: Evidence for phases of glacial modification of the dichotomy boundary. J. Geophys. Res. 112</ref> These lines may have developed as other glaciers moved down valleys. Some of these glaciers seem to come from material sitting around mesas and buttes.<ref>Baker, D., et al. 2009. 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> Lobate debris aprons (LDA) is the name given to these glaciers. All of these features that are believed to contain large amounts of ice are found in the mid-latitudes in both the Northern and Southern hemispheres.<ref>Marchant, D. and J. Head. 2007. Antarctic dry valleys: Microclimate zonation, variable geomorphic processes, and implications for assessing climatic change on Mars. Icarus: 192.187-222</ref> <ref>Dickson, J., et al. 2008. Late Amazonian glaciation at the dichotomy boundary on Mars: Evidence for glacial thickness maxima and multiple glacial phases. Geology: 36 (5) 411-415</ref> <ref>Kress, A., et al. 2006. The nature of the transition from lobate debris aprons to lineated valley fill: Mamers Valles, Northern Arabia Terra-Deuteronilus Mensae region on Mars. Lunar. Planet. Sci. 37. Abstract 1323</ref>

Suitupshowup: /* Polygonal Patterned Ground */ added ref about formation of polygons

2025-07-22T22:04:20Z

Polygonal Patterned Ground: added ref about formation of polygons

← Older revision		Revision as of 23:04, 22 July 2025
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	==Polygonal Patterned Ground==		==Polygonal Patterned Ground==

	Many surfaces on Mars display “polygonal patterned ground.” The polygons can be of different shapes and sizes. They are believed to be caused by ice in the ground.<ref>https://www.uahirise.org/ESP_047247_1150</ref> Like permafrost regions on Earth, this permanently frozen water is still active.		Many surfaces on Mars display “polygonal patterned ground.” The polygons can be of different shapes and sizes. They are believed to be caused by ice in the ground.<ref>https://www.uahirise.org/ESP_047247_1150</ref> Like permafrost regions on Earth, this permanently frozen water is still active.<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>

	With the changing seasons, alternate cooling and warming causes the ice-cemented soil to contract and expand. With the right conditions, cracks are made into the hard frozen ground releasing the stresses caused by contraction. Over long periods of cyclic cracking, a honeycomb-like polygonal pattern arises.<ref>https://www.uahirise.org/ESP_066782_1110</ref>		With the changing seasons, alternate cooling and warming causes the ice-cemented soil to contract and expand. With the right conditions, cracks are made into the hard frozen ground releasing the stresses caused by contraction. Over long periods of cyclic cracking, a honeycomb-like polygonal pattern arises.<ref>https://www.uahirise.org/ESP_066782_1110</ref>

Suitupshowup: /* Inverted relief */ added images of inverted terrain

2025-06-05T16:38:28Z

Inverted relief: added images of inverted terrain

← Older revision		Revision as of 17:38, 5 June 2025
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	[[File:ESP 077583 2255inverted.jpg\|thumb\|500px\|center\|Inverted stream, a stream bed has been filled with hard materials that did not erode away like the surroundings]]		[[File:ESP 077583 2255inverted.jpg\|thumb\|500px\|center\|Inverted stream, a stream bed has been filled with hard materials that did not erode away like the surroundings]]

			<gallery class="center" widths="380px" heights="360px">
			File:87429 1580invertedstreams2.jpg\|Curved ridge was once a stream, now it is a ridge becasuse it become filled with erosion-resistant materials. Later, the surrounding, softer ground became eroded. Image obtained through NASA's [[HiWish program]].

			File:87429 1580invertedstreams3.jpg\|Curved ridges were once streams, now they are ridges becasuse they become filled with erosion-resistant materials. Later, the surrounding, softer ground was eroded away.
			</gallery>

	==Troughs==		==Troughs==

Suitupshowup: /* Dark Slope Streaks */ added info and ref about streaks

2025-05-21T14:23:55Z

Dark Slope Streaks: added info and ref about streaks

← Older revision		Revision as of 15:23, 21 May 2025
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	Dark slope streaks are avalanche-like features common on dust-covered slopes, especially in the equatorial regions.<ref name=Chuang10>Chuang, F.C.; Beyer, R.A.; Bridges, N.T. (2010). Modification of Martian Slope Streaks by Eolian Processes. ''Icarus,'' '''205''' 154–164.</ref> These streaks have never been observed on the Earth.<ref>Heyer, T., et al. 2019. Seasonal formation rates of martian slope streaks. Icarus </ref>		Dark slope streaks are avalanche-like features common on dust-covered slopes, especially in the equatorial regions.<ref name=Chuang10>Chuang, F.C.; Beyer, R.A.; Bridges, N.T. (2010). Modification of Martian Slope Streaks by Eolian Processes. ''Icarus,'' '''205''' 154–164.</ref> These streaks have never been observed on the Earth.<ref>Heyer, T., et al. 2019. Seasonal formation rates of martian slope streaks. Icarus </ref>
	They form in relatively steep terrain, such as along cliffs and crater walls.<ref name= Schorghofer02>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> The darkest streaks are only about 10% darker than their surroundings. The streaks seem much darker because of contrast enhancement in the image processing.<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>		They form in relatively steep terrain, such as along cliffs and crater walls.<ref name= Schorghofer02>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> The darkest streaks are only about 10% darker than their surroundings. The streaks seem much darker because of contrast enhancement in the image processing.<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>

			Most beleive the streaks are just avalanches of bright dust. In a study of over 500,000 dark slope streaks, researchers found that streaks were more likey to form in dusty areas instead of moist places. The authors state: "We show that slope streaks modify less than 0.1% of the martian surface, but transport several global storm equivalents of dust per Mars year, potentially playing a major role in the martian dust cycle." <ref> Valentin, T. and A. Valantinas. 2025. Streaks on martian slopes are dry.
			Nature Communications. </ref> <ref>https://www.space.com/astronomy/mars/dark-streaks-on-mars-may-not-come-from-water-after-all-scientists-say?utm_term=CABA215D-3D47-4C9A-92FE-9ECF8D4C7909&lrh=e62336263a3610a07ef7c8af2080c758f2ecd0661aab1a8e6234cf31f0d0fdff&utm_campaign=58E4DE65-C57F-4CD3-9A5A-609994E2C5A9&utm_medium=email&utm_content=CC262A6E-5136-48F9-B124-6B5979B0DBA3&utm_source=SmartBrief</ref>

	Dry ice accumulates just under the surface during cold Martian nights and then changes to a gas in the morning. That gas creates enough wind to disturb dust particles and send them down steep slopes. As the bright dust slides down it reveals the underlying dark volcanic rocks. This process was discovered by measuring temperatures in the area. At the recorded temperatures, carbon dioxide from the air should have frozen on the surface, but it was not visible. It was concluded that the dry ice was forming just under the surface rather than on top..<ref>https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021JE006988</ref> <ref>Lange, S., et al. 2022. Gardening of the Martian Regolith by Diurnal CO2 Frost and the Formation of Slope Streaks. JGR Planets. Volume127, Issue4. e2021JE006988</ref>		Dry ice accumulates just under the surface during cold Martian nights and then changes to a gas in the morning. That gas creates enough wind to disturb dust particles and send them down steep slopes. As the bright dust slides down it reveals the underlying dark volcanic rocks. This process was discovered by measuring temperatures in the area. At the recorded temperatures, carbon dioxide from the air should have frozen on the surface, but it was not visible. It was concluded that the dry ice was forming just under the surface rather than on top..<ref>https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021JE006988</ref> <ref>Lange, S., et al. 2022. Gardening of the Martian Regolith by Diurnal CO2 Frost and the Formation of Slope Streaks. JGR Planets. Volume127, Issue4. e2021JE006988</ref>

Suitupshowup: /* Brain Terrain */ added info and ref about brain terrain

2025-05-03T19:14:34Z

Brain Terrain: added info and ref about brain terrain

← Older revision		Revision as of 20:14, 3 May 2025
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	==Brain Terrain==		==Brain Terrain==

	Brain terrain is a region of maze-like ridges 3–5 meters high. A person could wander between these ridges like a rat in a maze. Some ridges may consist of an ice core, so they may be sources of water for future colonists.<ref> Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.</ref>		Brain terrain is a region of maze-like ridges 3–5 meters high. It is one of the unsolved mysteries on Mars. This surface texture of interconnected ridges and troughs, referred to as “brain terrain” is found throughout the mid-latitude regions of Mars. A person could wander between these ridges like a rat in a maze. This bizarrely textured terrain may be directly related to the water-ice that lies beneath the surface.<ref>https://www.uahirise.org/ESP_058008_2225</ref> One hypothesis is that when the buried water-ice sublimates (changes from a solid to a gas), it forms the troughs in the ice. . Some ridges may consist of an ice core, so they may be sources of water for future colonists.<ref> Levy, J., J. Head, D. Marchant. 2009. Concentric crater fill in Utopia Planitia: History and interaction between glacial “brain terrain” and periglacial mantle processes. Icarus 202, 462–476.</ref>

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

Suitupshowup: /* Honeycomb Terrain */ added ref

2025-04-25T13:07:05Z

Honeycomb Terrain: added ref

← Older revision		Revision as of 14:07, 25 April 2025
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	[[File: ESP_049330_1425honeycomb.jpg\|thumb\|300px\|right\|Honeycomb terrain in Hellas quadrangle]]		[[File: ESP_049330_1425honeycomb.jpg\|thumb\|300px\|right\|Honeycomb terrain in Hellas quadrangle]]

	Honeycomb terrain is found on parts of the floor of Hellas Planitia. It may be due to rising bodies of ice followed by erosion.<ref>Bernhardt, H.; et al. (2016). "The honeycomb terrain on the Hellas basin floor, mars: a case for salt or ice diapirism: hellas honeycombs as salt/ice diapirs". J. Geophys. Res. 121: 714–738.</ref> <ref>Weiss, D., J. Head. 2017. HYDROLOGY OF THE HELLAS BASIN AND THE EARLY MARS CLIMATE: WAS THE HONEYCOMB TERRAIN FORMED BY SALT OR ICE DIAPIRISM? Lunar and Planetary Science XLVIII. 1060.pdf</ref> <ref>Weiss, D.; Head, J. (2017). "Salt or ice diapirism origin for the honeycomb terrain in Hellas basin, Mars?: Implications for the early martian climate". Icarus. 284: 249–263.</ref>		Honeycomb terrain is found on parts of the floor of Hellas Planitia. It may be due to rising bodies of ice followed by erosion.<ref>Bernhardt, H.; et al. (2016). "The honeycomb terrain on the Hellas basin floor, mars: a case for salt or ice diapirism: hellas honeycombs as salt/ice diapirs". J. Geophys. Res. 121: 714–738.</ref> <ref>Weiss, D., J. Head. 2017. HYDROLOGY OF THE HELLAS BASIN AND THE EARLY MARS CLIMATE: WAS THE HONEYCOMB TERRAIN FORMED BY SALT OR ICE DIAPIRISM? Lunar and Planetary Science XLVIII. 1060.pdf</ref> <ref>Weiss, D.; Head, J. (2017). "Salt or ice diapirism origin for the honeycomb terrain in Hellas basin, Mars?: Implications for the early martian climate". Icarus. 284: 249–263.</ref> Glaciers moving down slope may have been involved.<ref>https://www.uahirise.org/hipod/ESP_085926_1410</ref>


	<br clear=all>		<br clear=all>

	==Fractured Surface and Blocks==		==Fractured Surface and Blocks==

Suitupshowup: /* Gullies */ added image

2024-10-14T01:01:57Z

Gullies: added image

← Older revision		Revision as of 02:01, 14 October 2024
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	File:Close view of gullies ESP 080430 2310 01.jpg\|Gullies on crater wall The bright apron is a bit unusual.		File:Close view of gullies ESP 080430 2310 01.jpg\|Gullies on crater wall The bright apron is a bit unusual.
	File:Close view of gullies ESP 080430 2310 02.jpg\|Gully on crater wall The bright apron is a bit unusual.		File:Close view of gullies ESP 080430 2310 02.jpg\|Gully on crater wall The bright apron is a bit unusual.

			File:ESP 084659 1355 gullies cropped 01.jpg\|Wide view of gullies
			File:ESP 084659 1355 gullies cropped 02.jpg\|Close view of gully alcoves Picture is about 1 km across.
			File:ESP 084659 1355 gullies cropped 03.jpg\|Close view of gully alcoves Picture is about 1 km across.
			File:ESP 084659 1355 gullies cropped 04.jpg\|Close view of gully channels Picture is about 1 km across.
	</gallery>		</gallery>

← Older revision		Revision as of 02:01, 14 October 2024
Line 204:		Line 204:
	File:Close view of gullies ESP 080430 2310 01.jpg\|Gullies on crater wall The bright apron is a bit unusual.		File:Close view of gullies ESP 080430 2310 01.jpg\|Gullies on crater wall The bright apron is a bit unusual.
	File:Close view of gullies ESP 080430 2310 02.jpg\|Gully on crater wall The bright apron is a bit unusual.		File:Close view of gullies ESP 080430 2310 02.jpg\|Gully on crater wall The bright apron is a bit unusual.

			File:ESP 084659 1355 gullies cropped 01.jpg\|Wide view of gullies
			File:ESP 084659 1355 gullies cropped 02.jpg\|Close view of gully alcoves Picture is about 1 km across.
			File:ESP 084659 1355 gullies cropped 03.jpg\|Close view of gully alcoves Picture is about 1 km across.
			File:ESP 084659 1355 gullies cropped 04.jpg\|Close view of gully channels Picture is about 1 km across.
	</gallery>		</gallery>