Glaciers on Mars: Difference between revisions

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Glaciers, loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past.^[1]^[2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons, which show the characteristics of non-Newtonian flow, are now almost unanimously regarded as true glaciers.^[1]^[3]^[4]^[5]^[6]^[7]^[8]^[9]^[10]

However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain,^[1]^[11] lineated valley fill,^[12]^[9] concentric crater fill,^[3]^[13] and arcuate ridges.^[10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice.^[14]^[15]^[16]

Today, features interpreted as glaciers are largely restricted to latitudes polewards of around 30° latitude.^[17] Particular concentrations are found in the Ismenius Lacus quadrangle.^[2] Based on current models of the Martian atmosphere, ice should not be stable if exposed at the surface in the mid-Martian latitudes.^[18] It is thus thought that most glaciers must be covered with a layer of rubble or dust preventing free transfer of water vapor from the subliming ice into the air.^[8]^[18]^[19] This also suggests that in the recent geological past, the climate of Mars must have been different in order to allow the glaciers to grow stably at these latitudes.^[17] This provides good independent evidence that the obliquity of Mars has changed significantly in the past, as independently indicated by modelling of the orbit of Mars.^[20] Evidence for past glaciation also appears on the peaks of several Martian volcanoes in the tropics.^[21]^[22]^[23]

Like glaciers on Earth, glaciers on Mars are not pure water ice.^[1]^[10] Many are thought to contain substantial proportions of debris, and a substantial number are probably better described as rock glaciers.^[23]^[24]^[25] For many years, largely because of the modeled instability of water ice in the midlatitudes where the putative glacial features were concentrated, it was argued that almost all glaciers were rock glaciers on Mars.^[26] However, recent direct observations made by the SHARAD radar instrument on the Mars Reconnaissance Orbiter satellite have confirmed that at least some features are relatively pure ice, and thus, true glaciers.^[6]^[8] Some authors have also made claims that glaciers of solid carbon dioxide have formed on Mars under certain rare conditions.^[27]

Some landscapes look just like glaciers moving out of mountain valleys on Earth. Some appear to have a hollowed out center, looking like a glacier after almost all the ice has disappeared. What is left are the moraines—the dirt and debris carried by the glacier.^[28] These supposed alpine glaciers have been called glacier-like forms (GLF) or glacier-like flows (GLF).^[29] Glacier-like forms are a later and maybe more accurate term because we cannot be sure the structure is currently moving.^[30] Another, more general term sometimes seen in the literature is viscous flow features (VFF).^[30]

Radar studies

Radar studies with the SHAllow RADar (SHARAD) on the Mars Reconnaissance Orbiter showed that lobate debris aprons (LDA) and lineated valley fill (LVF) contain pure water ice covered with a thin layer of rocks that insulated the ice.^[31]^[32] Ice was found both in the southern hemisphere ^[33] and in the northern hemisphere.^[34] Researchers at the Niels Bohr Institute combined radar observations with ice flow modelling to say that ice in all of the Martian glaciers is equivalent to what could cover the entire surface of Mars with 1.1 meters of ice. The fact that the ice is still there suggests that a thick layer of dust is protecting the ice; the current atmospheric conditions on Mars are such that any exposed water ice would sublimate.^[35]^[36]^[37]

Martian glacier moving down a valley, as seen by HiRISE under HiWish program.

Climate changes

It is thought that ice accumulated when Mars' orbital tilt was very different from the present (the axis the planet spins on has considerable "wobble," meaning its angle changes over time).^[38]^[39]^[40] A few million years ago, the tilt of the axis of Mars was 45 degrees instead of its present 25 degrees. Its tilt, also called obliquity, varies greatly because its two tiny moons cannot stabilize it like the Moon stabilizes Earth.

Many features on Mars, especially in the Ismenius Lacus quadrangle, are believed to contain large amounts of ice. The most popular model for the origin of the ice is climate change from large changes in the tilt of the planet's rotational axis. At times the tilt has even been greater than 80 degrees^[41]^[42] Large changes in the tilt explains many ice-rich features on Mars.

Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.^[43] Furthermore, at this high tilt, stores of solid carbon dioxide (dry ice) sublimate, thereby increasing the atmospheric pressure. This increased pressure allows more dust to be held in the atmosphere. Moisture in the atmosphere will fall as snow or as ice frozen onto dust grains. Calculations suggest this material will concentrate in the mid-latitudes.^[44]^[45] General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found.^[42] When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.^[46]^[47] The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.^[48] The smooth surface mantle layer probably represents only relative recent material.

Geomorphology

Concentric crater fill, lineated valley fill, and lobate debris aprons

Several types of landforms have been identified as probably dirt and rock debris covering huge deposits of ice.^[49]^[50]^[51]^[52] 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.^[53]^[54] Lineated valley fill (LVF)are lines of ridges in valleys.^[55]^[56]^[57] 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.^[58] 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.^[59]^[60]^[61] These areas are sometimes called Fretted terrain because it is sometimes winkled. With the superior resolution of cameras on Mars Global Surveyor (MGS) and MRO, we have found the surface of LDA’s, LVF, and CCFs’ have a complex tangle of ridges that resemble the surface of the human brain. Wide ridges are called closed-cell brain terrain, and the less common narrow ridges are called open-cell brain terrain.^[62] It is thought that the wide closed-cell terrain still contains a core of ice, that when it eventually disappears the center of the wide ridge collapses to produce the narrow ridges of the open-cell brain terrain. Today it is widely accepted that glacier-like forms, lobate debris aprons, lineated valley fill, and concentric fill are all related in that they have the same surface texture. Glacier-like forms in valleys and cirque-like alcoves may coalesce with others to produce lobate debris aprons. When opposing lobate debris aprons converge, linear valley fill results ^[63]

Many of these features are found in the Northern hemisphere in parts of a boundary called the Martian dichotomy. The Martian dichotomy is mostly found between 0 and 70 E longitudes.^[64] Near this area are regions that are named from ancient names: Deuteronilus Mensae, Protonilus Mensae, and Nilosyrtis Mensae.

Well-developed hollows, as seen by HiRISE under the HiWish program. Hollows are on floor of a crater with concentric crater fill. Location is Casius quadrangle.
Close-up that shows cracks containing pits on the floor of a crater containing concentric crater fill, as seen by HiRISE under HiWish program. Location is Casius quadrangle.
Clanis and Hypsas Valles, as seen by HiRISE. Ridges are probably due to glacial flow. Ice is covered by a thin layer of rocks. Location is Ismenius Lacus quadrangle.
Coloe Fossae Lineated valley fill, as seen by HiRISE. Scale bar is 500 meters long. Location is Ismenius Lacus quadrangle.
Lineated valley fill in Ismenius Lacus quadrangle, as seen by HiRISE under HiWish program.
Close view of Lineated valley fill in Ismenius Lacus quadrangle, as seen by HiRISE under HiWish program
Close, color view of Lineated valley fill in Ismenius Lacus quadrangle, as seen by HiRISE under HiWish program
Valley showing Lineated valley fill, as seen by HiRISE under HiWish program Linear valley flow is caused by ice movements. Location is Casius quadrangle.
Lineated valley fill in valley, as seen by HiRISE under HiWish program Linear valley flow is ice covered by debris. Location is Ismenius Lacus quadrangle.
Close, color view of lineated valley fill, as seen by HiRISE under HiWish program
Lineated valley fill in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris. Picture is about 1 km wide.
Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
Lineated valley fill in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris. Picture is about 1 km wide.
This series of drawings illustrates why researchers believe many craters are full of ice-rich material. The depth of craters can be predicted based upon the observed diameter. Many craters are almost full, instead of having bowl shape; hence it is believed that they have gained much material since they were formed by impact. Much of the extra material is probably ice that fell from the sky as snow or ice-coated dust.
Wide CTX view of mesa showing lobate debris apron (LDA) and lineated valley fill. Both are believed to be debris-covered glaciers. Location is Ismenius Lacus quadrangle.
Close-up of lobate debris apron from the previous CTX image of a mesa. Image shows open-cell brain terrain and closed-cell brain terrain, which is more common. Open-cell brain terrain is thought to hold a core of ice. Image is from HiRISE under HiWish program.
Closed-cell brain terrain, as seen by HiRISE under the HiWish program. This type of surface is common on lobate debris aprons, concentric crater fill, and lineated valley fill.
Open and closed-cell brain terrain, as seen by HiRISE, under HiWish program.
Lobate debris aprons (LDAs) around a mesa, as seen by CTX. Mesa and LDAs are labeled so one can see their relationship. Radar studies have determined that LDAs contain ice; therefore these can be important for future colonists of Mars. Location is Ismenius Lacus quadrangle.
Close-up of lobate debris apron (LDA), as seen by HiRISE under HiWish program
Wide CTX view showing mesa and buttes with lobate debris aprons and lineated valley fill around them. Location is Ismenius Lacus quadrangle.
Lobate debris apron around mesa, as seen by HiRISE under HiWish program
Close view of lobate debris apron around mesa, as seen by HiRISE under HiWish program Brain terrain is visible.
Close-up of lineated valley fill (LVF), as seen by HiRISE under HiWish program Note: this is an enlargement of the previous CTX image.

Tongue-shaped glaciers

Some of the glaciers flow down mountains and are shaped by obstacles and valleys; they make a sort of tongue shape.^[65]

Tongue-shaped glacier, as seen by HiRISE under the HiWish program. Ice may exist in the glacier, even today, beneath an insulating layer of dirt. Location is Hellas quadrangle.
Tongue-shaped glacier, as seen by HiRISE under the HiWish program. Location is Phaethontis quadrangle.
Wide view of several tongue-shaped glaciers on wall of crater, as seen by HiRISE under the HiWish program. The glaciers are of different sizes and lie at different levels. Some of these are greatly enlarged in pictures which follow.
Close-up of the snouts of two glaciers from the previous image, as seen by HiRISE under the HiWish program. These are towards the bottom left of the previous image.
Close-up of small glaciers from a previous image, as seen by HiRISE under the HiWish program. Some of these glaciers seem to be just starting to form.
Close-up of the edge of one of the glaciers on the bottom of the wide view from a previous image Picture was taken by HiRISE under the HiWish program.
Close-up of tongue-shaped glacier, as seen by HiRISE under the HiWish program. Resolution is about 1 meter, so one can see objects a few meters across in this image. Ice may exist in the glacier, even today, beneath an insulating layer of dirt. Location is Hellas quadrangle.
Tongue-shaped glaciers indicated with arrows, as seen by HiRISE under the HiWish program
Close view of snout of glacier, as seen by HiRISE under the HiWish program High center polygons are visible. Box shows size of football field.
Close view of high center polygons near glacier, as seen by HiRISE under the HiWish program
Close view of high center polygons near glacier, as seen by HiRISE under the HiWish program Box shows size of football field.
Close view of high center polygons near glacier, as seen by HiRISE under the HiWish program
Wide view of tongue-shaped flows, as seen by HiRISE under the HiWish program
Close view of tongue-shaped flows, as seen by HiRISE under the HiWish program
Close view of tongue-shaped flows and polygonal terrain (which is labeled), as seen by HiRISE under the HiWish program
Close view of polygonal terrain near tongue-shaped flows, as seen by HiRISE under the HiWish program

Hummocky relief

A hummocky relief resembling Northern Sweden's Veiki moraines has been found in Nereidum Montes. The relief is hypothesized to result from the melting of a Martian glacier.^[66]

There is no current evidence of any glaciers on any of the volcanoes on Mars

Ice sheet

There is much evidence for a large ice sheet that existed in the south polar region of the planet.^[67]^[68]^[69]^[70] A large number of eskers which form under ice are found there. The field of eskers make up the Dorsa Argentea Formation. The ice sheet had an area twice that of the state of Texas.^[71]

Evidence also is building up for the past existence of an ice sheet in the Tharsis region.^[72] ^[73] ^[74] ^[75] ^[76] It would have been in the Late Hesperian time period. When it melted it may have helped to form a northern ocean.^[77] ^[78] ^[79] ^[80]

Ridges, believed to be eskers of the Dorsa Argentea Formation, as seen by Mars Global Surveyor wide angle MOC. White arrows point to the ridges.

Ground ice

Mars has vast glaciers hidden under a layer of rocky debris over wide areas in the mid-latitudes. These glaciers could be large reservoir of life-supporting water on the planet for simple life forms and for future colonists.^[83] Research by John Holt, of the University of Texas at Austin, and others found that one of the features examined is three times larger than the city of Los Angeles and up to 800 m thick, and there are many more.^[84]^[85]

Some of the glacial-like features were revealed by NASA's Viking orbiters in the 1970s. Since that time glacial-like features have been studied by more and more advanced instruments. Much better data has been received from Mars Global Surveyor, Mars Odyssey, Mars Express, and Mars Reconnaissance Orbiter.

Gallery

Moreux Crater moraines and kettle holes, as seen by HIRISE. Location is Ismenius Lacus quadrangle.
Surface showing appearance with and without mantle covering, as seen by HiRISE, under the HiWish program. Location is Terra Sirenum in Phaethontis quadrangle. Mantle fell from the sky and may be a major source of ice for glaciers.
Glacier moving out of valley, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Romer Lake's Elephant Foot Glacier in the Earth's Arctic, as seen by Landsat 8. This picture shows several glaciers that have the same shape as many features on Mars that are believed to also be glaciers.
Glacier coming out of valley, as seen by HiRISE under HiWish program Location is rim of Moreux Crater. Location is Ismenius Lacus quadrangle.
The arrow in the left picture points to a possibly valley carved by a glacier. The image on the right shows the valley greatly enlarged in a Mars Global Surveyor image.
Gullies and possible remains of old glaciers in a crater in Eridania quadrangle, north of the large crater Kepler. One suspected glacier, to the right, has the shape of a tongue. Image was taken by the Mars Global Surveyor under the Public Target program.
Mesa in Ismenius Lacus quadrangle, as seen by CTX. Mesa has several glaciers eroding it. One of the glaciers is seen in greater detail in the next two images from HiRISE. Image from Ismenius Lacus quadrangle.
Glacier as seen by HiRISE under the HiWish program. Area in rectangle is enlarged in the next photo. Zone of accumulation of snow at the top. Glacier is moving down valley, then spreading out on plain. Evidence for flow comes from the many lines on surface. Location is in Protonilus Mensae in Ismenius Lacus quadrangle.
Enlargement of area in rectangle of the previous image. Interpreted as the terminal moraine of a glacier. Picture taken with HiRISE under the HiWish program. Image from Ismenius Lacus quadrangle.
Context for the next image of the end of a flow feature or glacier. Location is Hellas quadrangle. Picture taken with HiRISE under the HiWish program.
Close-up of the area in the box in the previous image. Interpreted as the terminal moraine of a glacier. For scale, the box shows the approximate size of a football field. Image taken with HiRISE under the HiWish program. Location is Hellas quadrangle.
Possible moraine on the end of a past glacier on a mound in Deuteronilus Mensae, as seen by HiRISE, under the HiWish program.
Possible Glacial Cirque in Hellas Planitia, as seen by HiRISE, under the HiWish program. Lines are probably due to downhill movement.
Glaciers, as seen by HiRISE, under HiWish program. Glacier on left is thin because it has lost much of its ice. Glacier on the right on the other hand is thick; it still contains a lot of ice that is under a thin layer of dirt and rock. Location is Hellas quadrangle.
Remains of glaciers, as seen by HiRISE under the HiWish program. Image from Ismenius Lacus quadrangle.
Probable glacier as seen by HiRISE under HiWish program. Radar studies have found that it is made up of almost totally of pure ice. It appears to be moving from the high ground (a mesa) on the right. Location is Ismenius Lacus quadrangle.
Tributary Glacier, as seen by HiRISE. Location is Ismenius Lacus quadrangle.
Arrows point to drumlin-like shapes that were probably formed under a glacier, as seen by HiRISE, under HiWish program. Some of the shapes require liquid water under the glacier to form. Location is Ismenius Lacus quadrangle.
Glacier on a crater floor, as seen by HiRISE under HiWish program The cracks in the glacier may be crevasses. There is also a gully system on the crater wall. Location is Casius quadrangle.
Glacier, as seen by HiRISE under HiWish program Location is Casius quadrangle.
Glaciers moving in two different valleys, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Wide view of flow moving down valley, as seen by HiRISE under HiWish program Location is Ismenius Lacus quadrangle.
Close view of part of glacier, as seen by HiRISE under HiWish program Box shows size of football field. Location is Ismenius Lacus quadrangle.
Grooves caused by movement of glacier, as seen by HiRISE under HiWish program
Close, color view of polygons, as seen by HiRISE under HiWish program Polygons are common in ice-rich ground.

Interactive Mars map

References

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^ Madeleine, J. et al. 2007. Mars: A proposed climatic scenario for northern mid-latitude glaciation. Lunar Planet. Sci. 38. Abstract 1778.
^ Madeleine, J. et al. 2009. Amazonian northern mid-latitude glaciation on Mars: A proposed climate scenario. Icarus: 203. 300-405.
^ Mischna, M. et al. 2003. On the orbital forcing of martian water and CO2 cycles: A general circulation model study with simplified volatile schemes. J. Geophys. Res. 108. (E6). 5062.
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External links

Martian Ice - Jim Secosky - 16th Annual International Mars Society Convention
https://www.youtube.com/watch?v=kpnTh3qlObk[T. Gordon Wasilewski - Water on Mars - 20th Annual International Mars Society Convention] Describes how to get water from ice in the ground
High resolution flyover video by Seán Doran of a glacier in Protonilus Mensae, based on NASA digital terrain model; see album for more
Jeffrey Plaut - Subsurface Ice - 21st Annual International Mars Society Convention

[Carr-1] "The Surface of Mars" Series: Cambridge Planetary Science (No. 6) ISBN 978-0-511-26688-1 Michael H. Carr, United States Geological Survey, Menlo Park

[Kieffer1992-2] Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved March 7, 2011.

[Milliken-3] Milliken, R. E.; Mustard, J. F.; Goldsby, D. L. (2003). "Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images". Journal of Geophysical Research. 108 (E6): 5057. Bibcode:2003JGRE..108.5057M. doi:10.1029/2002je002005.

[SquyresCarr-4] Squyres, S.W.; Carr, M.H. (1986). "Geomorphic evidence for the distribution of ground ice on Mars". Science. 213 (4735): 249–253. Bibcode:1986Sci...231..249S. doi:10.1126/science.231.4735.249. PMID 17769645. S2CID 34239136.

[Headetal2010-5] Head, J.W.; Marchant, D.R.; Dickson, J.L.; Kress, A.M. (2010). "Criteria for the recognition of debris-covered glacier and valley glacier landsystem deposits". Earth Planet. Sci. Lett. 294 (3–4): 306–320. Bibcode:2010E&PSL.294..306H. doi:10.1016/j.epsl.2009.06.041.

[HoltetalSHARAD-6] Holt, J.W.; et al. (2008). "Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars". Science. 322 (5905): 1235–1238. Bibcode:2008Sci...322.1235H. doi:10.1126/science.1164246. hdl:11573/67950. PMID 19023078. S2CID 36614186.

[MorganetalDeuteronilus-7] Morgan, G.A.; Head, J.W.; Marchant, D.R. (2009). "Lineated valley fill (LVF) and lobate debris aprons (LDA) in the Deuteronilus Mensae northern dichotomy boundary region, Mars: Constraints on the extent, age and episodicity of Amazonian glacial events". Icarus. 202 (1): 22–38. Bibcode:2009Icar..202...22M. doi:10.1016/j.icarus.2009.02.017.

[Plautetal-8] Plaut, J.J.; Safaeinili, A.; Holt, J.W.; Phillips, R.J.; Head, J.W.; Sue, R.; Putzig, A. (2009). "Frigeri Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars". Geophys. Res. Lett. 36: L02203. doi:10.1029/2008gl036379. S2CID 17530607.

[Bakeretal2010-9] Baker, D.M.H.; Head, J.W.; Marchant, D.R. (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 (1): 186–209. Bibcode:2010Icar..207..186B. doi:10.1016/j.icarus.2009.11.017.

[ArfstromHartmann-10] Arfstrom, J. (2005). "Terrestrial analogs and interrelationships". Icarus. 174 (2): 321–335. Bibcode:2005Icar..174..321A. doi:10.1016/j.icarus.2004.05.026.

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[LevyBrainTerrain-13] Levy, Joseph S.; Head, James W.; Marchant, David R. (2009). "Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial mantle processes". Icarus. 202 (2): 462–476. Bibcode:2009Icar..202..462L. doi:10.1016/j.icarus.2009.02.018.

[Hubbard-14] Hubbard, Bryn; et al. (2011). "Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars". Icarus. 211 (1): 330–346. Bibcode:2011Icar..211..330H. doi:10.1016/j.icarus.2010.10.021.

[15] Arfstrom, J (2005). "Terrestrial analogs and interrelationships". Icarus. 174 (2): 321–335. Bibcode:2005Icar..174..321A. doi:10.1016/j.icarus.2004.05.026.

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[28] Milliken, R.; Mustard, J.; Goldsby, D. (2003). "Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images". J. Geophys. Res. 108 (E6): 5057. Bibcode:2003JGRE..108.5057M. doi:10.1029/2002JE002005.

[29] Arfstrom, J; Hartmann, W. (2005). "Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships". Icarus. 174 (2): 321–335. Bibcode:2005Icar..174..321A. doi:10.1016/j.icarus.2004.05.026.

[Hubbard_B._2011-30] Hubbard, B.; Milliken, R.; Kargel, J.; Limaye, A.; Souness, C. (2011). "Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars". Icarus. 211 (1): 330–346. Bibcode:2011Icar..211..330H. doi:10.1016/j.icarus.2010.10.021.

[Plaut,_J._2008-31] Plaut, J. et al. 2008. Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars. Lunar and Planetary Science XXXIX. 2290.pdf

[32] "HiRISE | Merging Lobate Debris Aprons of Deuteronilus Mensae (PSP_009535_2240)".

[33] Holt, J.; Safaeinili, A.; Plaut, J.; Head, J.; Phillips, R.; Seu, R.; Kempf, S.; Choudhary, P.; Young, D.; Putzig, N.; Biccari, D.; Gim, Y. (2008). "Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars". Science. 322 (5905): 1235–1238. Bibcode:2008Sci...322.1235H. doi:10.1126/science.1164246. hdl:11573/67950. PMID 19023078. S2CID 36614186.

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[43] Levy, J.; Head, J.; Marchant, D.; Kowalewski, D. (2008). "Identification of sublimation-type thermal contraction crack polygons at the proposed NASA Phoenix landing site: Implications for substrate properties and climate-driven morphological evolution". Geophys. Res. Lett. 35 (4): L04202. Bibcode:2008GeoRL..35.4202L. doi:10.1029/2007GL032813.

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+{{Short description|Extraterrestrial bodies of ice}}
-[[File:Wide view of glacier showing image field.JPG|thumb|Martian glacier as seen by HiRISE. Glacier is moving down valley, then spreading out on plain. Evidence for flow comes from the many lines on surface. The rimming ridges at the end of the glacier are probably [[moraine]]s. Location is in [[Protonilus Mensae]] in [[Ismenius Lacus quadrangle]].]]
+[[File:Wide view of glacier showing image field.JPG|thumb|Martian glacier as seen by HiRISE. Glacier is moving down valley, then spreading out on plain. Evidence for flow comes from the many lines on surface. The rimming ridges at the end of the glacier are probably [[moraine]]s Location is in [[Protonilus Mensae]] in [[Ismenius Lacus quadrangle]].]]
-[[Glaciers]], loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past.<ref name="Carr">"The Surface of Mars" Series: Cambridge Planetary Science (No. 6) {{ISBN|978-0-511-26688-1}}  Michael H. Carr, United States Geological Survey, Menlo Park</ref><ref name="Kieffer1992">{{cite book|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|accessdate=March 7, 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref> Lobate convex features on the surface known as viscous flow features and [[lobate debris aprons]], which show the characteristics of [[Non-Newtonian fluid|non-Newtonian flow]], are now almost unanimously regarded as true glaciers.<ref name="Carr" /><ref name="Milliken">{{cite journal | last1 = Milliken | first1 = R. E. | last2 = Mustard | first2 = J. F. | last3 = Goldsby | first3 = D. L. | year = 2003 | title = Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images | url = | journal = Journal of Geophysical Research | volume = 108 | issue = E6| page = 5057 | doi=10.1029/2002je002005 | bibcode=2003JGRE..108.5057M}}</ref><ref name="SquyresCarr">{{cite journal | last1 = Squyres | first1 = S.W. | last2 = Carr | first2 = M.H. | year = 1986 | title = Geomorphic evidence for the distribution of ground ice on Mars | url = https://zenodo.org/record/1230966| journal = Science | volume = 213 | issue = 4735| pages = 249–253 | doi = 10.1126/science.231.4735.249 | pmid = 17769645 | bibcode = 1986Sci...231..249S | s2cid = 34239136 }}</ref><ref name="Headetal2010">{{cite journal | last1 = Head | first1 = J.W. | last2 = Marchant | first2 = D.R. | last3 = Dickson | first3 = J.L. | last4 = Kress | first4 = A.M. | year = 2010 | title = Criteria for the recognition of debris-covered glacier and valley glacier landsystem deposits | url = | journal = Earth Planet. Sci. Lett. | volume = 294 | issue = | pages = 306–320 | doi=10.1016/j.epsl.2009.06.041 | bibcode=2010E&PSL.294..306H}}</ref><ref name="HoltetalSHARAD">{{cite journal | last1 = Holt | first1 = J.W. |display-authors=etal | year = 2008 | title = Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars | url = | journal = Science | volume = 322 | issue = 5905| pages = 1235–1238 | doi=10.1126/science.1164246 | pmid=19023078| bibcode = 2008Sci...322.1235H | s2cid = 36614186 }}</ref><ref name="MorganetalDeuteronilus">{{cite journal | last1 = Morgan | first1 = G.A. | last2 = Head | first2 = J.W. | last3 = Marchant | first3 = D.R. | year = 2009 | title = Lineated valley fill (LVF) and lobate debris aprons (LDA) in the Deuteronilus Mensae northern dichotomy boundary region, Mars: Constraints on the extent, age and episodicity of Amazonian glacial events | url = | journal = Icarus | volume = 202 | issue = 1| pages = 22–38 | doi=10.1016/j.icarus.2009.02.017 | bibcode=2009Icar..202...22M}}</ref><ref name="Plautetal">{{cite journal | last1 = Plaut | first1 = J.J. | last2 = Safaeinili | first2 = A. | last3 = Holt | first3 = J.W. | last4 = Phillips | first4 = R.J. | last5 = Head | first5 = J.W. | last6 = Sue | first6 = R. | last7 = Putzig | first7 = A. | year = 2009 | title = Frigeri Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars | doi = 10.1029/2008gl036379 | journal = Geophys. Res. Lett. | volume = 36 | issue = | page = L02203 | bibcode=2009GeoRL..3602203P}}</ref><ref name="Bakeretal2010">{{cite journal | last1 = Baker | first1 = D.M.H. | last2 = Head | first2 = J.W. | last3 = Marchant | first3 = D.R. | year = 2010 | title = 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 | url = | journal = Icarus | volume = 207 | issue = 1| pages = 186–209 | doi=10.1016/j.icarus.2009.11.017 | bibcode=2010Icar..207..186B}}</ref><ref name="ArfstromHartmann">{{cite journal | last1 = Arfstrom | first1 = J. | year = 2005 | title = Terrestrial analogs and interrelationships | url = | journal = Icarus | volume = 174 | issue = | pages = 321–335 | doi=10.1016/j.icarus.2004.05.026 | bibcode=2005Icar..174..321A}}</ref>
+[[Glaciers]], loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past.<ref name="Carr">"The Surface of Mars" Series: Cambridge Planetary Science (No. 6) {{ISBN|978-0-511-26688-1}}  Michael H. Carr, United States Geological Survey, Menlo Park</ref><ref name="Kieffer1992">{{cite book|author=Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ|access-date=March 7, 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7}}</ref> Lobate convex features on the surface known as viscous flow features and [[lobate debris aprons]], which show the characteristics of [[Non-Newtonian fluid|non-Newtonian flow]], are now almost unanimously regarded as true glaciers.<ref name="Carr" /><ref name="Milliken">{{cite journal | last1 = Milliken | first1 = R. E. | last2 = Mustard | first2 = J. F. | last3 = Goldsby | first3 = D. L. | year = 2003 | title = Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images | journal = Journal of Geophysical Research | volume = 108 | issue = E6| page = 5057 | doi=10.1029/2002je002005 | bibcode=2003JGRE..108.5057M}}</ref><ref name="SquyresCarr">{{cite journal | last1 = Squyres | first1 = S.W. | last2 = Carr | first2 = M.H. | year = 1986 | title = Geomorphic evidence for the distribution of ground ice on Mars | url = https://zenodo.org/record/1230966| journal = Science | volume = 213 | issue = 4735| pages = 249–253 | doi = 10.1126/science.231.4735.249 | pmid = 17769645 | bibcode = 1986Sci...231..249S | s2cid = 34239136 }}</ref><ref name="Headetal2010">{{cite journal | last1 = Head | first1 = J.W. | last2 = Marchant | first2 = D.R. | last3 = Dickson | first3 = J.L. | last4 = Kress | first4 = A.M. | year = 2010 | title = Criteria for the recognition of debris-covered glacier and valley glacier landsystem deposits | journal = Earth Planet. Sci. Lett. | volume = 294 | issue = 3–4 | pages = 306–320 | doi=10.1016/j.epsl.2009.06.041 | bibcode=2010E&PSL.294..306H}}</ref><ref name="HoltetalSHARAD">{{cite journal | last1 = Holt | first1 = J.W. |display-authors=etal | year = 2008 | title = Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars | journal = Science | volume = 322 | issue = 5905| pages = 1235–1238 | doi=10.1126/science.1164246 | pmid=19023078| bibcode = 2008Sci...322.1235H | hdl = 11573/67950 | s2cid = 36614186 }}</ref><ref name="MorganetalDeuteronilus">{{cite journal | last1 = Morgan | first1 = G.A. | last2 = Head | first2 = J.W. | last3 = Marchant | first3 = D.R. | year = 2009 | title = Lineated valley fill (LVF) and lobate debris aprons (LDA) in the Deuteronilus Mensae northern dichotomy boundary region, Mars: Constraints on the extent, age and episodicity of Amazonian glacial events | journal = Icarus | volume = 202 | issue = 1| pages = 22–38 | doi=10.1016/j.icarus.2009.02.017 | bibcode=2009Icar..202...22M}}</ref><ref name="Plautetal">{{cite journal | last1 = Plaut | first1 = J.J. | last2 = Safaeinili | first2 = A. | last3 = Holt | first3 = J.W. | last4 = Phillips | first4 = R.J. | last5 = Head | first5 = J.W. | last6 = Sue | first6 = R. | last7 = Putzig | first7 = A. | year = 2009 | title = Frigeri Radar evidence for ice in lobate debris aprons in the mid-northern latitudes of Mars | doi = 10.1029/2008gl036379 | journal = Geophys. Res. Lett. | volume = 36 | page = L02203 | s2cid = 17530607 | doi-access = free }}</ref><ref name="Bakeretal2010">{{cite journal | last1 = Baker | first1 = D.M.H. | last2 = Head | first2 = J.W. | last3 = Marchant | first3 = D.R. | year = 2010 | title = 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 | journal = Icarus | volume = 207 | issue = 1| pages = 186–209 | doi=10.1016/j.icarus.2009.11.017 | bibcode=2010Icar..207..186B}}</ref><ref name="ArfstromHartmann">{{cite journal | last1 = Arfstrom | first1 = J. | year = 2005 | title = Terrestrial analogs and interrelationships | journal = Icarus | volume = 174 | issue = 2 | pages = 321–335 | doi=10.1016/j.icarus.2004.05.026 | bibcode=2005Icar..174..321A}}</ref>
-However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as [[fretted terrain]],<ref name="Carr" /><ref name="Luchitta">{{cite journal | last1 = Lucchitta | first1 = Baerbel K | year = 1984 | title = Ice and debris in the fretted terrain, Mars | url = | journal = Journal of Geophysical Research: Solid Earth | volume = 89 | issue = S02| pages = B409–B418 | doi=10.1029/jb089is02p0b409 | bibcode=1984LPSC...14..409L}}</ref>  [[lineated valley fill]],<ref>{{cite journal | last1 = Lucchitta | first1 = Baerbel K | year = 1984 | title = Ice and debris in the fretted terrain, Mars | url = | journal = Journal of Geophysical Research: Solid Earth | volume = 89 | issue = | pages = B409–B418 | doi = 10.1029/jb089is02p0b409 | bibcode = 1984LPSC...14..409L }}</ref><ref name="Bakeretal2010" /> [[concentric crater fill]],<ref name="Milliken" /><ref name="LevyBrainTerrain">{{cite journal | last1 = Levy | first1 = Joseph S. | last2 = Head | first2 = James W. | last3 = Marchant | first3 = David R. | year = 2009 | title = Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial mantle processes | url = | journal = Icarus | volume = 202 | issue = 2| pages = 462–476 | doi=10.1016/j.icarus.2009.02.018 | bibcode=2009Icar..202..462L}}</ref> and arcuate ridges.<ref name="ArfstromHartmann" />  A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice.<ref name="Hubbard">{{cite journal | last1 = Hubbard | first1 = Bryn |display-authors=etal | year = 2011 | title = Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars | url = | journal = Icarus | volume = 211 | issue = 1| pages = 330–346 | doi=10.1016/j.icarus.2010.10.021 | bibcode=2011Icar..211..330H}}</ref><ref>{{cite journal | last1 = Arfstrom | first1 = J | year = 2005 | title = Terrestrial analogs and interrelationships | url = | journal = Icarus | volume = 174 | issue = | pages = 321–335 | doi = 10.1016/j.icarus.2004.05.026 | bibcode = 2005Icar..174..321A }}</ref><ref>Arfstrom, J., W. Hartmann.  2018.  THE CAUSES OF VISCOUS FLOW SURFACE PATTERNS AT CRATER GREG AND DAO VALLIS.  49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).  1156.pdf</ref>
+However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as [[fretted terrain]],<ref name="Carr" /><ref name="Luchitta">{{cite journal | last1 = Lucchitta | first1 = Baerbel K | year = 1984 | title = Ice and debris in the fretted terrain, Mars | journal = Journal of Geophysical Research: Solid Earth | volume = 89 | issue = S02| pages = B409–B418 | doi=10.1029/jb089is02p0b409 | bibcode=1984LPSC...14..409L}}</ref>  [[lineated valley fill]],<ref>{{cite journal | last1 = Lucchitta | first1 = Baerbel K | year = 1984 | title = Ice and debris in the fretted terrain, Mars | journal = Journal of Geophysical Research: Solid Earth | volume = 89 | pages = B409–B418 | doi = 10.1029/jb089is02p0b409 | bibcode = 1984LPSC...14..409L }}</ref><ref name="Bakeretal2010" /> [[concentric crater fill]],<ref name="Milliken" /><ref name="LevyBrainTerrain">{{cite journal | last1 = Levy | first1 = Joseph S. | last2 = Head | first2 = James W. | last3 = Marchant | first3 = David R. | year = 2009 | title = Concentric crater fill in Utopia Planitia: History and interaction between glacial "brain terrain" and periglacial mantle processes | journal = Icarus | volume = 202 | issue = 2| pages = 462–476 | doi=10.1016/j.icarus.2009.02.018 | bibcode=2009Icar..202..462L}}</ref> and arcuate ridges.<ref name="ArfstromHartmann" />  A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice.<ref name="Hubbard">{{cite journal | last1 = Hubbard | first1 = Bryn |display-authors=etal | year = 2011 | title = Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars | journal = Icarus | volume = 211 | issue = 1| pages = 330–346 | doi=10.1016/j.icarus.2010.10.021 | bibcode=2011Icar..211..330H| doi-access = free }}</ref><ref>{{cite journal | last1 = Arfstrom | first1 = J | year = 2005 | title = Terrestrial analogs and interrelationships | journal = Icarus | volume = 174 | issue = 2 | pages = 321–335 | doi = 10.1016/j.icarus.2004.05.026 | bibcode = 2005Icar..174..321A }}</ref><ref>Arfstrom, J., W. Hartmann.  2018.  THE CAUSES OF VISCOUS FLOW SURFACE PATTERNS AT CRATER GREG AND DAO VALLIS.  49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083).  1156.pdf</ref>
-Today, features interpreted as glaciers are largely restricted to latitudes polewards of around 30° latitude.<ref name="HeadDistn">{{cite journal | last1 = Head | first1 = J. W. |display-authors=etal | year = 2006 | title = Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change | url = | journal = Earth and Planetary Science Letters | volume = 241 | issue = 3| pages = 663–671 | doi=10.1016/j.epsl.2005.11.016 | bibcode=2006E&PSL.241..663H}}</ref> Particular concentrations are found in the [[Ismenius Lacus quadrangle]].<ref name="Kieffer1992" /> Based on current models of the [[Atmosphere of Mars|Martian atmosphere]], ice should not be stable if exposed at the surface in the mid-Martian latitudes.<ref name="WilliamsSnowpack">{{cite journal | last1 = Williams | first1 = K. E. |display-authors=etal | year = 2008 | title = Stability of mid-latitude snowpacks on Mars | url = | journal = Icarus | volume = 196 | issue = 2| pages = 565–577 | doi=10.1016/j.icarus.2008.03.017 | bibcode=2008Icar..196..565W}}</ref> It is thus thought that most glaciers must be covered with a layer of rubble or dust preventing free transfer of water vapor from the subliming ice into the air.<ref name="Plautetal" /><ref name="WilliamsSnowpack" /><ref name="Head, J. 2005">{{cite journal | doi = 10.1038/nature03359 | last1 = Head | first1 = J. | date = 2005 | last2 = Neukum | first2 = G. | last3 = Jaumann | first3 = R. | last4 = Hiesinger | first4 = H. | last5 = Hauber | first5 = E. | last6 = Carr | first6 = M. | last7 = Masson | first7 = P. | last8 = Foing | first8 = B. | last9 = Hoffmann | first9 = H. | last10 = Kreslavsky | first10 = M. | last11 = Werner | first11 = S.|author11-link= Stephanie C. Werner | last12 = Milkovich | first12 = S. | last13 = Van Gasselt | first13 = S. | last14 = Co-Investigator Team | first14 = The Hrsc
+Today, features interpreted as glaciers are largely restricted to latitudes polewards of around 30° latitude.<ref name="HeadDistn">{{cite journal | last1 = Head | first1 = J. W. |display-authors=etal | year = 2006 | title = Extensive valley glacier deposits in the northern mid-latitudes of Mars: Evidence for Late Amazonian obliquity-driven climate change | journal = Earth and Planetary Science Letters | volume = 241 | issue = 3| pages = 663–671 | doi=10.1016/j.epsl.2005.11.016 | bibcode=2006E&PSL.241..663H}}</ref> Particular concentrations are found in the [[Ismenius Lacus quadrangle]].<ref name="Kieffer1992" /> Based on current models of the [[Atmosphere of Mars|Martian atmosphere]], ice should not be stable if exposed at the surface in the mid-Martian latitudes.<ref name="WilliamsSnowpack">{{cite journal | last1 = Williams | first1 = K. E. |display-authors=etal | year = 2008 | title = Stability of mid-latitude snowpacks on Mars | journal = Icarus | volume = 196 | issue = 2| pages = 565–577 | doi=10.1016/j.icarus.2008.03.017 | bibcode=2008Icar..196..565W}}</ref> It is thus thought that most glaciers must be covered with a layer of rubble or dust preventing free transfer of water vapor from the subliming ice into the air.<ref name="Plautetal" /><ref name="WilliamsSnowpack" /><ref name="Head, J. 2005">{{cite journal | doi = 10.1038/nature03359 | last1 = Head | first1 = J. | date = 2005 | last2 = Neukum | first2 = G. | last3 = Jaumann | first3 = R. | last4 = Hiesinger | first4 = H. | last5 = Hauber | first5 = E. | last6 = Carr | first6 = M. | last7 = Masson | first7 = P. | last8 = Foing | first8 = B. | last9 = Hoffmann | first9 = H. | last10 = Kreslavsky | first10 = M. | last11 = Werner | first11 = S.|author11-link= Stephanie C. Werner | last12 = Milkovich | first12 = S. | last13 = Van Gasselt | first13 = S. | last14 = Co-Investigator Team | first14 = The Hrsc
  | title = Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars
- | url = | journal=Nature | volume = 434 | issue = 7031| pages = 346–350 | pmid=15772652|bibcode = 2005Natur.434..346H | s2cid = 4363630 | display-authors = 8 }}</ref> This also suggests that in the recent geological past, the [[climate of Mars]] must have been different in order to allow the glaciers to grow stably at these latitudes.<ref name="HeadDistn" /> This provides good independent evidence that the [[obliquity]] of Mars has changed significantly in the past, as independently indicated by modelling of the [[orbit of Mars]].<ref name="Laskar">{{cite journal | last1 = Laskar | first1 = Jacques |display-authors=etal | year = 2004
+ | journal=Nature | volume = 434 | issue = 7031| pages = 346–350 | pmid=15772652|bibcode = 2005Natur.434..346H | s2cid = 4363630 | display-authors = 8 }}</ref> This also suggests that in the recent geological past, the [[climate of Mars]] must have been different in order to allow the glaciers to grow stably at these latitudes.<ref name="HeadDistn" /> This provides good independent evidence that the [[obliquity]] of Mars has changed significantly in the past, as independently indicated by modelling of the [[orbit of Mars]].<ref name="Laskar">{{cite journal | last1 = Laskar | first1 = Jacques |display-authors=etal | year = 2004
  | title = Long term evolution and chaotic diffusion of the insolation quantities of Mars
  | url = https://hal.archives-ouvertes.fr/hal-00000860/file/Ma_2004.laskar_prep.pdf| journal = Icarus | volume = 170 | issue = 2| pages = 343–364
- | doi=10.1016/j.icarus.2004.04.005 | bibcode=2004Icar..170..343L}}</ref> Evidence for past glaciation also appears on the peaks of several Martian volcanoes in the tropics.<ref name="HeadTropical">{{cite journal | last1 = Head | first1 = J. W. |display-authors=etal | year = 2005 | title = Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars | url = | journal = Nature | volume = 434 | issue = 7031| pages = 346–351 | doi=10.1038/nature03359 | pmid=15772652| bibcode = 2005Natur.434..346H | s2cid = 4363630 }}</ref><ref name="SheanPavonis">{{cite journal | last1 = Shean | first1 = David E. | title = Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit | journal=Journal of Geophysical Research | volume = 110 | issue = E5 | pages = E05001 | date = 2005 | doi = 10.1029/2004JE002360 | bibcode=2005JGRE..110.5001S}}</ref><ref name="HeadMarchantArsia">{{cite journal | last1 = Head | first1 = James W. | last2 = Marchant | first2 = David R. | year = 2003 | title = Cold-based mountain glaciers on Mars: western Arsia Mons | url = | journal = Geology | volume = 31 | issue = 7| pages = 641–644 | doi=10.1130/0091-7613(2003)031<0641:cmgomw>2.0.co;2| bibcode = 2003Geo....31..641H }}</ref>
+ | doi=10.1016/j.icarus.2004.04.005 | bibcode=2004Icar..170..343L| s2cid = 33657806 }}</ref> Evidence for past glaciation also appears on the peaks of several Martian volcanoes in the tropics.<ref name="HeadTropical">{{cite journal | last1 = Head | first1 = J. W. |display-authors=etal | year = 2005 | title = Tropical to mid-latitude snow and ice accumulation, flow and glaciation on Mars | journal = Nature | volume = 434 | issue = 7031| pages = 346–351 | doi=10.1038/nature03359 | pmid=15772652| bibcode = 2005Natur.434..346H | s2cid = 4363630 }}</ref><ref name="SheanPavonis">{{cite journal | last1 = Shean | first1 = David E. | title = Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit | journal=Journal of Geophysical Research | volume = 110 | issue = E5 | pages = E05001 | date = 2005 | doi = 10.1029/2004JE002360 | bibcode=2005JGRE..110.5001S| doi-access = free }}</ref><ref name="HeadMarchantArsia">{{cite journal | last1 = Head | first1 = James W. | last2 = Marchant | first2 = David R. | year = 2003 | title = Cold-based mountain glaciers on Mars: western Arsia Mons | journal = Geology | volume = 31 | issue = 7| pages = 641–644 | doi=10.1130/0091-7613(2003)031<0641:cmgomw>2.0.co;2| bibcode = 2003Geo....31..641H }}</ref>
-Like glaciers on Earth, glaciers on Mars are not pure water ice.<ref name="Carr" /><ref name="ArfstromHartmann" /> Many are thought to contain substantial proportions of debris, and a substantial number are probably better described as [[rock glacier]]s.<ref name="HeadMarchantArsia" /><ref>Colaprete, Anthony, and Bruce M. Jakosky. "Ice flow and rock glaciers on Mars." ''Journal of Geophysical Research: Planets'' 103.E3 (1998): 5897-5909.</ref><ref>{{cite journal | last1 = Haeberli | first1 = Wilfried |display-authors=etal | year = 2006 | title = Permafrost creep and rock glacier dynamics | url = | journal = [[Permafrost and Periglacial Processes]] | volume = 17 | issue = 3| pages = 189–214 | doi=10.1002/ppp.561}}</ref> For many years, largely because of the modeled instability of water ice in the midlatitudes where the putative glacial features were concentrated, it was argued that almost all glaciers were rock glaciers on Mars.<ref>{{cite journal | last1 = Squyres | first1 = Steven W | year = 1978 | title = Martian fretted terrain: Flow of erosional debris | url = | journal = Icarus | volume = 34 | issue = 3| pages = 600–613 | doi=10.1016/0019-1035(78)90048-9 | bibcode=1978Icar...34..600S}}</ref> However, recent direct observations made by the [[SHARAD]] radar instrument on the [[Mars Reconnaissance Orbiter]] satellite have confirmed that at least some features are relatively pure ice, and thus, true glaciers.<ref name="HoltetalSHARAD" /><ref name="Plautetal" /> Some authors have also made claims that glaciers of solid carbon dioxide have formed on Mars under certain rare conditions.<ref name="KreslavskyHeadCO2">{{cite journal
+Like glaciers on Earth, glaciers on Mars are not pure water ice.<ref name="Carr" /><ref name="ArfstromHartmann" /> Many are thought to contain substantial proportions of debris, and a substantial number are probably better described as [[rock glacier]]s.<ref name="HeadMarchantArsia" /><ref>Colaprete, Anthony, and Bruce M. Jakosky. "Ice flow and rock glaciers on Mars." ''Journal of Geophysical Research: Planets'' 103.E3 (1998): 5897-5909.</ref><ref>{{cite journal | last1 = Haeberli | first1 = Wilfried |display-authors=etal | year = 2006 | title = Permafrost creep and rock glacier dynamics | journal = [[Permafrost and Periglacial Processes]] | volume = 17 | issue = 3| pages = 189–214 | doi=10.1002/ppp.561| bibcode = 2006PPPr...17..189H | s2cid = 130188056 }}</ref> For many years, largely because of the modeled instability of water ice in the midlatitudes where the putative glacial features were concentrated, it was argued that almost all glaciers were rock glaciers on Mars.<ref>{{cite journal | last1 = Squyres | first1 = Steven W | year = 1978 | title = Martian fretted terrain: Flow of erosional debris | journal = Icarus | volume = 34 | issue = 3| pages = 600–613 | doi=10.1016/0019-1035(78)90048-9 | bibcode=1978Icar...34..600S}}</ref> However, recent direct observations made by the [[SHARAD]] radar instrument on the ''[[Mars Reconnaissance Orbiter]]'' satellite have confirmed that at least some features are relatively pure ice, and thus, true glaciers.<ref name="HoltetalSHARAD" /><ref name="Plautetal" /> Some authors have also made claims that glaciers of solid carbon dioxide have formed on Mars under certain rare conditions.<ref name="KreslavskyHeadCO2">{{cite journal
  | last1 = Kreslavsky | first1 = Mikhail A.
  | last2 = Head | first2 = James W. | year = 2011
  | title = Carbon dioxide glaciers on Mars: Products of recent low obliquity epochs (?)
- | url = | journal = Icarus | volume = 216 | issue = 1| pages = 111–115
+ | journal = Icarus | volume = 216 | issue = 1| pages = 111–115
  | doi=10.1016/j.icarus.2011.08.020 | bibcode=2011Icar..216..111K}}</ref>
-Some landscapes look just like glaciers moving out of mountain valleys on Earth.  Some appear to have a hollowed out center, looking like a glacier after almost all the ice has disappeared.  What is left are the [[moraine]]s—the dirt and debris carried by the glacier.<ref>{{cite journal | last1 = Milliken | first1 = R. | last2 = Mustard | first2 = J. | last3 = Goldsby | first3 = D. | year = 2003 | title = Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images | url = | journal = J. Geophys. Res. | volume =  108| issue = E6| page =  5057| doi = 10.1029/2002JE002005 | bibcode = 2003JGRE..108.5057M }}</ref>   These supposed alpine glaciers have been called glacier-like forms (GLF) or glacier-like flows (GLF).<ref>{{cite journal
+Some landscapes look just like glaciers moving out of mountain valleys on Earth.  Some appear to have a hollowed out center, looking like a glacier after almost all the ice has disappeared.  What is left are the [[moraine]]s—the dirt and debris carried by the glacier.<ref>{{cite journal | last1 = Milliken | first1 = R. | last2 = Mustard | first2 = J. | last3 = Goldsby | first3 = D. | year = 2003 | title = Viscous flow features on the surface of Mars: Observations from high-resolution Mars Orbiter Camera (MOC) images | journal = J. Geophys. Res. | volume =  108| issue = E6| page =  5057| doi = 10.1029/2002JE002005 | bibcode = 2003JGRE..108.5057M }}</ref>   These supposed alpine glaciers have been called glacier-like forms (GLF) or glacier-like flows (GLF).<ref>{{cite journal
  | last1 = Arfstrom | first1 = J
  | last2 = Hartmann | first2 = W. | year = 2005
  | title = Martian flow features, moraine-like ridges, and gullies: Terrestrial analogs and interrelationships
- | url = | journal = Icarus | volume = 174 | issue = 2| pages = 321–335
+ | journal = Icarus | volume = 174 | issue = 2| pages = 321–335
  | doi=10.1016/j.icarus.2004.05.026 | bibcode=2005Icar..174..321A}}</ref>   Glacier-like forms are a later and maybe more accurate term because we cannot be sure the structure is currently moving.<ref name="Hubbard B. 2011">{{cite journal
  | last1 = Hubbard | first1 = B.
@@ Line 30: / Line 31: @@
  | last5 = Souness | first5 = C.
  | year = 2011 | title = Geomorphological characterisation and interpretation of a mid-latitude glacier-like form: Hellas Planitia, Mars
- | url = | journal = Icarus | volume = 211 | issue = 1| pages = 330–346
+ | journal = Icarus | volume = 211 | issue = 1| pages = 330–346
- | doi=10.1016/j.icarus.2010.10.021 | bibcode=2011Icar..211..330H}}</ref>  Another, more general term sometimes seen in the literature is viscous flow features (VFF).<ref name="Hubbard B. 2011"/>
+ | doi=10.1016/j.icarus.2010.10.021 | bibcode=2011Icar..211..330H| doi-access = free}}</ref>  Another, more general term sometimes seen in the literature is viscous flow features (VFF).<ref name="Hubbard B. 2011"/>
 <!---
 <gallery class="center"  widths="190px" heights="180px" >
@@ Line 39: / Line 40: @@
 ==Radar studies==
-Radar studies with the SHAllow RADar (SHARAD) on the [[Mars Reconnaissance Orbiter]] showed that lobate debris aprons (LDA) and lineated valley fill (LVF) contain pure water ice covered with a thin layer of rocks that insulated the ice.<ref name="Plaut, J. 2008">Plaut, J. et al.  2008. Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars. Lunar and Planetary Science XXXIX.  2290.pdf</ref><ref>http://hirise.lpl.arizona.edu/PSP_009535_2240</ref> Ice was found both in the southern hemisphere <ref>{{cite journal | last1 = Holt | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Plaut | first3 = J. | last4 = Head | first4 = J. | last5 = Phillips | first5 = R. | last6 = Seu | first6 = R. | last7 = Kempf | first7 = S. | last8 = Choudhary | first8 = P. | last9 = Young | first9 = D. | last10 = Putzig | first10 = N. | last11 = Biccari | first11 = D. | last12 = Gim | first12 = Y. | year = 2008 | title = Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars | url = | journal = Science | volume =  322| issue = 5905| pages =  1235–1238| doi = 10.1126/science.1164246 | pmid=19023078| bibcode = 2008Sci...322.1235H | s2cid = 36614186 }}</ref> and in the northern hemisphere.<ref>{{cite journal | last1 = Plaut | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Holt | first3 = J. | last4 = Phillips | first4 = R. | last5 = Head | first5 = J. | last6 = Seu | first6 = R. | last7 = Putzig | first7 = N. | last8 = Frigeri | first8 = A. | year = 2009 | title = Radar evidence for ice in lobate debris aprons in the midnorthern latitudes of Mars | url = | journal = Geophys. Res. Lett. | volume =  36| issue = 2| pages = n/a | doi = 10.1029/2008GL036379 | bibcode=2009GeoRL..3602203P}}</ref>  Researchers at the Niels Bohr Institute combined radar observations with ice flow modelling to say that ice in all of the Martian glaciers is equivalent to what could cover the entire surface of Mars with 1.1 meters of ice.  The fact that the ice is still there suggests that a thick layer of dust is protecting the ice; the current atmospheric conditions on Mars are such that any exposed water ice would sublimate.<ref>http://spaceref.com/mars/mars-has-belts-of-glaciers-consisting-of-frozen-water.html</ref><ref>https://www.sciencedaily.com/releases/2015/04/150408102701.htm</ref><ref>{{cite journal | last1 = Karlsson | first1 = N. | last2 = Schmidt | first2 = L. | last3 = Hvidberg | first3 = C. | year = 2015 | title = Volume of Martian mid-latitude glaciers from radar observations and ice-flow modelling | url = | journal = Geophysical Research Letters | volume =  42| issue = 8| pages =  2627–2633| doi = 10.1002/2015GL063219 | bibcode = 2015GeoRL..42.2627K}}</ref>
+Radar studies with the SHAllow RADar (SHARAD) on the ''[[Mars Reconnaissance Orbiter]]'' showed that lobate debris aprons (LDA) and lineated valley fill (LVF) contain pure water ice covered with a thin layer of rocks that insulated the ice.<ref name="Plaut, J. 2008">Plaut, J. et al.  2008. Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars. ''Lunar and Planetary Science'' XXXIX.  2290.pdf</ref><ref>{{Cite web|url=http://hirise.lpl.arizona.edu/PSP_009535_2240|title=HiRISE &#124; Merging Lobate Debris Aprons of Deuteronilus Mensae (PSP_009535_2240)}}</ref> Ice was found both in the southern hemisphere <ref>{{cite journal | last1 = Holt | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Plaut | first3 = J. | last4 = Head | first4 = J. | last5 = Phillips | first5 = R. | last6 = Seu | first6 = R. | last7 = Kempf | first7 = S. | last8 = Choudhary | first8 = P. | last9 = Young | first9 = D. | last10 = Putzig | first10 = N. | last11 = Biccari | first11 = D. | last12 = Gim | first12 = Y. | year = 2008 | title = Radar sounding evidence for buried glaciers in the southern mid-latitudes of Mars | journal = Science | volume =  322| issue = 5905| pages =  1235–1238| doi = 10.1126/science.1164246 | pmid=19023078| bibcode = 2008Sci...322.1235H | hdl = 11573/67950 | s2cid = 36614186 }}</ref> and in the northern hemisphere.<ref>{{cite journal | last1 = Plaut | first1 = J. | last2 = Safaeinili | first2 = A. | last3 = Holt | first3 = J. | last4 = Phillips | first4 = R. | last5 = Head | first5 = J. | last6 = Seu | first6 = R. | last7 = Putzig | first7 = N. | last8 = Frigeri | first8 = A. | year = 2009 | title = Radar evidence for ice in lobate debris aprons in the midnorthern latitudes of Mars | journal = Geophys. Res. Lett. | volume =  36| issue = 2| pages = n/a | doi = 10.1029/2008GL036379 | s2cid = 17530607 | doi-access = free | bibcode = 2009GeoRL..36.2203P }}</ref>  Researchers at the Niels Bohr Institute combined radar observations with ice flow modelling to say that ice in all of the Martian glaciers is equivalent to what could cover the entire surface of Mars with 1.1 meters of ice.  The fact that the ice is still there suggests that a thick layer of dust is protecting the ice; the current atmospheric conditions on Mars are such that any exposed water ice would sublimate.<ref>{{Cite web|url=http://spaceref.com/mars/mars-has-belts-of-glaciers-consisting-of-frozen-water.html|archive-url=https://archive.today/20150409145413/http://spaceref.com/mars/mars-has-belts-of-glaciers-consisting-of-frozen-water.html|url-status=dead|archive-date=April 9, 2015|title=Mars Has Belts of Glaciers Consisting of Frozen Water - SpaceRef|date=8 April 2015}}</ref><ref>{{Cite web|url=https://www.sciencedaily.com/releases/2015/04/150408102701.htm|title = Ice on Mars: Mars has belts of glaciers consisting of frozen water}}</ref><ref>{{cite journal | last1 = Karlsson | first1 = N. | last2 = Schmidt | first2 = L. | last3 = Hvidberg | first3 = C. | year = 2015 | title = Volume of Martian mid-latitude glaciers from radar observations and ice-flow modelling | journal = Geophysical Research Letters | volume =  42| issue = 8| pages =  2627–2633| doi = 10.1002/2015GL063219 | bibcode = 2015GeoRL..42.2627K| s2cid = 129648554 | doi-access = free }}</ref>
 {{wide image|ESP 028352 2245glacier.jpg|600px|align-cap=center|Martian glacier moving down a valley, as seen by HiRISE under HiWish program.}}
@@ Line 45: / Line 46: @@
 ==Climate changes==
 {{Further|Water on Mars#Ice ages}}
-It is thought that ice accumulated when Mars' orbital tilt was very different from the present (the axis the planet spins on has considerable "wobble," meaning its angle changes over time).<ref>Madeleine, J. et al. 2007.  Mars:  A proposed climatic scenario for northern mid-latitude glaciation.  Lunar Planet. Sci. 38.  Abstract 1778.</ref><ref>Madeleine, J. et al.  2009.  Amazonian northern mid-latitude glaciation on Mars:  A proposed climate scenario.  Icarus: 203. 300-405.</ref><ref>Mischna, M. et al.  2003.  On the orbital forcing of martian water and CO2 cycles:  A general circulation model study with simplified volatile schemes.  J. Geophys. Res.  108. (E6).  5062.</ref>  A few million years ago, the tilt of the axis of Mars was 45 degrees instead of its present 25 degrees.  Its tilt, also called obliquity, varies greatly because its two tiny moons cannot stabilize it like our moon.
+It is thought that ice accumulated when Mars' orbital tilt was very different from the present (the axis the planet spins on has considerable "wobble," meaning its angle changes over time).<ref>Madeleine, J. et al. 2007.  Mars:  A proposed climatic scenario for northern mid-latitude glaciation.  Lunar Planet. Sci. 38.  Abstract 1778.</ref><ref>Madeleine, J. et al.  2009.  Amazonian northern mid-latitude glaciation on Mars:  A proposed climate scenario.  Icarus: 203. 300-405.</ref><ref>Mischna, M. et al.  2003.  On the orbital forcing of martian water and CO2 cycles:  A general circulation model study with simplified volatile schemes.  J. Geophys. Res.  108. (E6).  5062.</ref>  A few million years ago, the tilt of the axis of Mars was 45 degrees instead of its present 25 degrees.  Its tilt, also called obliquity, varies greatly because its two tiny moons cannot stabilize it like the Moon stabilizes Earth.
-Many features on Mars, especially in the Ismenius Lacus quadrangle, are believed to contain large amounts of ice.  The most popular model for the origin of the ice is climate change from large changes in the tilt of the planet's rotational axis.  At times the tilt has even been greater than 80 degrees<ref>{{cite journal | last1 = Touma | first1 = J. | last2 = Wisdom | first2 = J. | year = 1993 | title = The Chaotic Obliquity of Mars | url = | journal = Science | volume = 259 | issue = 5099| pages = 1294–1297 | doi=10.1126/science.259.5099.1294 | pmid=17732249| bibcode = 1993Sci...259.1294T | s2cid = 42933021 }}</ref><ref name="ReferenceB">{{cite journal | last1 = Laskar | first1 = J. | last2 = Correia | first2 = A. | last3 = Gastineau | first3 = M. | last4 = Joutel | first4 = F. | last5 = Levrard | first5 = B. | last6 = Robutel | first6 = P. | year = 2004 | title = Long term evolution and chaotic diffusion of the insolation quantities of Mars | url = https://hal.archives-ouvertes.fr/hal-00000860/file/Ma_2004.laskar_prep.pdf| journal = Icarus | volume = 170 | issue = 2| pages = 343–364 | doi=10.1016/j.icarus.2004.04.005 | bibcode=2004Icar..170..343L}}</ref>   Large changes in the tilt explains many ice-rich features on Mars.
+Many features on Mars, especially in the Ismenius Lacus quadrangle, are believed to contain large amounts of ice.  The most popular model for the origin of the ice is climate change from large changes in the tilt of the planet's rotational axis.  At times the tilt has even been greater than 80 degrees<ref>{{cite journal | last1 = Touma | first1 = J. | last2 = Wisdom | first2 = J. | year = 1993 | title = The Chaotic Obliquity of Mars | journal = Science | volume = 259 | issue = 5099| pages = 1294–1297 | doi=10.1126/science.259.5099.1294 | pmid=17732249| bibcode = 1993Sci...259.1294T | s2cid = 42933021 }}</ref><ref name="ReferenceB">{{cite journal | last1 = Laskar | first1 = J. | last2 = Correia | first2 = A. | last3 = Gastineau | first3 = M. | last4 = Joutel | first4 = F. | last5 = Levrard | first5 = B. | last6 = Robutel | first6 = P. | year = 2004 | title = Long term evolution and chaotic diffusion of the insolation quantities of Mars | url = https://hal.archives-ouvertes.fr/hal-00000860/file/Ma_2004.laskar_prep.pdf| journal = Icarus | volume = 170 | issue = 2| pages = 343–364 | doi=10.1016/j.icarus.2004.04.005 | bibcode=2004Icar..170..343L| s2cid = 33657806 }}</ref>   Large changes in the tilt explains many ice-rich features on Mars.
-Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | last4 = Kowalewski | first4 = D. | year = 2008 | title = Identification of sublimation-type thermal contraction crack polygons at the proposed NASA Phoenix landing site: Implications for substrate properties and climate-driven morphological evolution | url = | journal = Geophys. Res. Lett. | volume =  35| issue = 4| pages = L04202 | doi = 10.1029/2007GL032813 | bibcode = 2008GeoRL..35.4202L }}</ref>   Furthermore, at this high tilt, stores of solid carbon dioxide (dry ice) sublimate, thereby increasing the atmospheric pressure.  This increased pressure allows more dust to be held in the atmosphere.  Moisture in the atmosphere will fall as snow or as ice frozen onto dust grains.  Calculations suggest this material will concentrate in the mid-latitudes.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | year = 2009a | title = Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations | url = | journal = J. Geophys. Res. | volume =  114| issue = E1| pages = E01007 | doi = 10.1029/2008JE003273 | bibcode = 2009JGRE..114.1007L }}</ref><ref>Hauber, E., D. Reiss, M. Ulrich, F. Preusker, F. Trauthan, M. Zanetti, H. Hiesinger, R. Jaumann, L. Johansson, A. Johnsson, S. Van Gaselt, M. Olvmo.  2011.  Landscape evolution in Martian mid-latitude regions:  insights from analogous periglacial landforms in Svalbard.  In: Balme, M., A. Bargery, C. Gallagher, S. Guta (eds). Martian Geomorphology.  Geological Society, London.  Special Publications: 356.  111-131</ref>  General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found.<ref name="ReferenceB"/>
+Studies have shown that when the tilt of Mars reaches 45 degrees from its current 25 degrees, ice is no longer stable at the poles.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | last4 = Kowalewski | first4 = D. | year = 2008 | title = Identification of sublimation-type thermal contraction crack polygons at the proposed NASA Phoenix landing site: Implications for substrate properties and climate-driven morphological evolution | journal = Geophys. Res. Lett. | volume =  35| issue = 4| pages = L04202 | doi = 10.1029/2007GL032813 | bibcode = 2008GeoRL..35.4202L | doi-access = free }}</ref>   Furthermore, at this high tilt, stores of solid carbon dioxide (dry ice) sublimate, thereby increasing the atmospheric pressure.  This increased pressure allows more dust to be held in the atmosphere.  Moisture in the atmosphere will fall as snow or as ice frozen onto dust grains.  Calculations suggest this material will concentrate in the mid-latitudes.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | year = 2009a | title = Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations | journal = J. Geophys. Res. | volume =  114| issue = E1| pages = E01007 | doi = 10.1029/2008JE003273 | bibcode = 2009JGRE..114.1007L | doi-access = free }}</ref><ref>Hauber, E., D. Reiss, M. Ulrich, F. Preusker, F. Trauthan, M. Zanetti, H. Hiesinger, R. Jaumann, L. Johansson, A. Johnsson, S. Van Gaselt, M. Olvmo.  2011.  Landscape evolution in Martian mid-latitude regions:  insights from analogous periglacial landforms in Svalbard.  In: Balme, M., A. Bargery, C. Gallagher, S. Guta (eds). Martian Geomorphology.  Geological Society, London.  Special Publications: 356.  111-131</ref>  General circulation models of the Martian atmosphere predict accumulations of ice-rich dust in the same areas where ice-rich features are found.<ref name="ReferenceB"/>
-When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.<ref name="Mellon, M. 1995">{{cite journal | last1 = Mellon | first1 = M. | last2 = Jakosky | first2 = B. | year = 1995 | title = The distribution and behavior of Martian ground ice during past and present epochs | url = | journal = J. Geophys. Res. | volume = 100 | issue = E6| pages = 11781–11799 | doi=10.1029/95je01027 | bibcode=1995JGR...10011781M}}</ref><ref name="Mellon, M. 1995"/><ref>{{cite journal | last1 = Schorghofer | first1 = N | year = 2007 | title = Dynamics of ice ages on Mars | url = | journal = Nature | volume = 449 | issue = 7159| pages = 192–194 | doi=10.1038/nature06082 | pmid=17851518| bibcode = 2007Natur.449..192S| s2cid = 4415456 }}</ref>   The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.<ref>Madeleine, J., F. Forget, J. Head, B. Levrard, F. Montmessin. 2007.  Exploring the northern mid-latitude glaciation with a general circulation model.  In:  Seventh International Conference on Mars.  Abstract 3096.</ref>   The smooth surface mantle layer probably represents only relative recent material.
+When the tilt begins to return to lower values, the ice sublimates (turns directly to a gas) and leaves behind a lag of dust.<ref name="Mellon, M. 1995">{{cite journal | last1 = Mellon | first1 = M. | last2 = Jakosky | first2 = B. | year = 1995 | title = The distribution and behavior of Martian ground ice during past and present epochs | journal = J. Geophys. Res. | volume = 100 | issue = E6| pages = 11781–11799 | doi=10.1029/95je01027 | bibcode=1995JGR...10011781M}}</ref><ref>{{cite journal | last1 = Schorghofer | first1 = N | year = 2007 | title = Dynamics of ice ages on Mars | journal = Nature | volume = 449 | issue = 7159| pages = 192–194 | doi=10.1038/nature06082 | pmid=17851518| bibcode = 2007Natur.449..192S| s2cid = 4415456 }}</ref>   The lag deposit caps the underlying material so with each cycle of high tilt levels, some ice-rich mantle remains behind.<ref>Madeleine, J., F. Forget, J. Head, B. Levrard, F. Montmessin. 2007.  Exploring the northern mid-latitude glaciation with a general circulation model.  In:  Seventh International Conference on Mars.  Abstract 3096.</ref>   The smooth surface mantle layer probably represents only relative recent material.
 ==Geomorphology==
 ===Concentric crater fill, lineated valley fill, and lobate debris aprons===
-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 debrid.  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>  These areas are sometimes called [[Fretted terrain]] because it is sometimes winkled.  With the superior resolution of cameras on Mars Global Surveyor (MGS) and MRO, we have found the surface of LDA’s, LVF, and CCFs’ have a complex tangle of ridges that resemble the surface of the human brain.  Wide ridges are called closed-cell [[brain terrain]], and the less common narrow ridges are called open-cell brain terrain.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | year = 2009 | title = Concentric crater fill in Utopia Planitia: History and interaction between glacial ''brain terrain'' and periglacial mantle processes | url = | journal = Icarus | volume = 202 | issue = 2| pages = 462–476 | doi=10.1016/j.icarus.2009.02.018 | bibcode=2009Icar..202..462L}}</ref>  It is thought that the wide closed-cell terrain still contains a core of ice, that when it eventually disappears the center of the wide ridge collapses to produce the narrow ridges of the open-cell brain terrain.
+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 NASA.gov]</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 debrid.  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>  These areas are sometimes called [[Fretted terrain]] because it is sometimes winkled.  With the superior resolution of cameras on Mars Global Surveyor (MGS) and MRO, we have found the surface of LDA’s, LVF, and CCFs’ have a complex tangle of ridges that resemble the surface of the human brain.  Wide ridges are called closed-cell [[brain terrain]], and the less common narrow ridges are called open-cell brain terrain.<ref>{{cite journal | last1 = Levy | first1 = J. | last2 = Head | first2 = J. | last3 = Marchant | first3 = D. | year = 2009 | title = Concentric crater fill in Utopia Planitia: History and interaction between glacial ''brain terrain'' and periglacial mantle processes | journal = Icarus | volume = 202 | issue = 2| pages = 462–476 | doi=10.1016/j.icarus.2009.02.018 | bibcode=2009Icar..202..462L}}</ref>  It is thought that the wide closed-cell terrain still contains a core of ice, that when it eventually disappears the center of the wide ridge collapses to produce the narrow ridges of the open-cell brain terrain.
-Today it is widely accepted that glacier-like forms, lobate debris aprons, lineated valley fill, and concentric fill are all related in that they have the same surface texture.  Glacier-like forms in valleys and cirque-like alcoves may coalesce with others to produce lobate debris aprons.  When opposing lobate debris aprons converge, linear valley fill results <ref>{{cite journal | last1 = Souness | first1 = C. | last2 = Hubbard | first2 = B. | year = 2013 | title = An alternative interpretation of late Amazonian ice flow: Protonilus Mensae, Mars | url = | journal = Icarus | volume = 225 | issue = 1| pages = 495–505 | doi=10.1016/j.icarus.2013.03.030 | bibcode=2013Icar..225..495S}}</ref>
+Today it is widely accepted that glacier-like forms, lobate debris aprons, lineated valley fill, and concentric fill are all related in that they have the same surface texture.  Glacier-like forms in valleys and cirque-like alcoves may coalesce with others to produce lobate debris aprons.  When opposing lobate debris aprons converge, linear valley fill results <ref>{{cite journal | last1 = Souness | first1 = C. | last2 = Hubbard | first2 = B. | year = 2013 | title = An alternative interpretation of late Amazonian ice flow: Protonilus Mensae, Mars | journal = Icarus | volume = 225 | issue = 1| pages = 495–505 | doi=10.1016/j.icarus.2013.03.030 | bibcode=2013Icar..225..495S}}</ref>
 Many of these features are found in the Northern hemisphere in parts of a boundary called the [[Martian dichotomy]]. The Martian dichotomy is mostly found between 0 and 70 E longitudes.<ref>Barlow, N.  2008.  Mars:  An Introduction to its Interior, Surface and Atmosphere.  Cambridge University Press.  {{ISBN|978-0-521-85226-5}}</ref>  Near this area are regions that are named from ancient names: [[Deuteronilus Mensae]], [[Protonilus Mensae]], and [[Nilosyrtis Mensae]].
-<gallery class="center"  widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 Image:Hollows as seen by hirise under hiwish program.jpg|Well-developed hollows, as seen by HiRISE under the [[HiWish program]].  Hollows are on floor of a crater with concentric crater fill.  Location is [[Casius quadrangle]].
 Image:crackswithpitsconcentric.jpg|Close-up that shows cracks containing pits on the floor of a crater containing concentric crater fill, as seen by HiRISE under HiWish program.  Location is [[Casius quadrangle]].
@@ Line 74: / Line 75: @@
 ESP 050137 2185lvfclosecolor.jpg|Close, color view of lineated valley fill, as seen by HiRISE under HiWish program
+File:ESP 084607 2210lvf 01.jpg|Lineated valley fill in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
+File:ESP 084607 2210lvf 02.jpg|Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.  Picture is about 1 km wide.
+File:ESP 084607 2210lvf 03.jpg|Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
+File:ESP 084607 2210lvf 04.jpg|Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
+File:ESP 084607 2210lvf 05.jpg|Lineated valley fill in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.
+File:ESP 084607 2210lvf 06.jpg|Close view of lineated valley fill (LVF) in valley, as seen by HiRISE under HiWish program. Linear valley flow is ice covered by debris.  Picture is about 1 km wide.
 File:Ccffigurecaptioned.jpg|This series of drawings illustrates why researchers believe many craters are full of ice-rich material.  The depth of craters can be predicted based upon the observed diameter.  Many craters are almost full, instead of having bowl shape; hence it is believed that they have gained much material since they were formed by impact.  Much of the extra material is probably ice that fell from the sky as snow or ice-coated dust.
@@ Line 93: / Line 101: @@
 === Tongue-shaped glaciers ===
 Some of the glaciers flow down mountains and are shaped by obstacles and valleys; they make a sort of tongue shape.<ref>Forget, F., et al.  2006.  Planet Mars Story of Another World.  Praxis Publishing, Chichester, UK.  {{ISBN|978-0-387-48925-4}}</ref>
-<gallery class="center"  widths="190px" heights="180px" >
+<gallery class="center"  widths="380px" heights="360px">
 Image:Tongue23141.jpg|Tongue-shaped glacier, as seen by HiRISE under the HiWish program.  Ice may exist in the glacier, even today, beneath an insulating layer of dirt.  Location is [[Hellas quadrangle]].
 ESP 036995 1410tongue.jpg|Tongue-shaped glacier, as seen by HiRISE under the HiWish program.  Location is [[Phaethontis quadrangle]].
@@ Line 113: / Line 122: @@
 ===Hummocky relief===
-A hummocky relief resembling [[Norrland terrain|Northern Sweden's]] [[Veiki moraine]]s has been found in [[Nereidum Montes]]. The relief is hypothesized to result from the melting of a Martian glacier.<ref>{{cite conference |url=http://elib.dlr.de/110003/1/Johnsson_et_al.Veiki_Moraines.LPSC_2016.1229.pdf |title=Veiki-moraine-like Landforms in the Nereidum Montes Region on Mars: Insights from Analogues in Northern Sweden |last1=Johnsson |first1=A.  |last2=Reiss |first2=D. |last3=Hauber |first3=E. |last4=Johnson |first4=M.D.|last5=Olvmo |first5=M.|last6=Hiesinger |first6=H. |date=2016 |book-title= |pages= |location= |conference=47th Lunar and Planetary Science Conference|id= }}</ref>
+A hummocky relief resembling [[Norrland terrain|Northern Sweden's]] [[Veiki moraine]]s has been found in [[Nereidum Montes]]. The relief is hypothesized to result from the melting of a Martian glacier.<ref>{{cite conference |url=http://elib.dlr.de/110003/1/Johnsson_et_al.Veiki_Moraines.LPSC_2016.1229.pdf |title=Veiki-moraine-like Landforms in the Nereidum Montes Region on Mars: Insights from Analogues in Northern Sweden |last1=Johnsson |first1=A.  |last2=Reiss |first2=D. |last3=Hauber |first3=E. |last4=Johnson |first4=M.D.|last5=Olvmo |first5=M.|last6=Hiesinger |first6=H. |date=2016 |conference=47th Lunar and Planetary Science Conference}}</ref>
+There is no current evidence of any glaciers on any of the volcanoes on Mars
-== Glaciers on volcanoes ==
-Many suspected glaciers have been observed on some large Martian volcanoes.  Researchers have described glacial deposits on [[Hecates Tholus]],<ref name="Hauber, E. 2005">{{Cite journal|author=Hauber, E. |date=2005 |title=Discovery of a flank caldera and very young glacial activity at Hecates Tholus, Mars |journal=Nature |volume=434 |pages=356–61|pmid=15772654|issue=7031|doi=10.1038/nature03423|bibcode = 2005Natur.434..356H |last2=Van Gasselt |first2=Stephan |last3=Ivanov |first3=Boris |last4=Werner |first4=Stephanie |author4-link= Stephanie C. Werner |last5=Head |first5=James W. |last6=Neukum |first6=Gerhard |last7=Jaumann |first7=Ralf |last8=Greeley |first8=Ronald |last9=Mitchell |first9=Karl L. |last10=Muller |first10=Peter |last11=Co-Investigator Team |first11=The Hrsc |s2cid=4427179 }}</ref> [[Arsia Mons]],<ref>Scanlon, K., J. Head, D. Marchant.  2015. REMNANT BURIED ICE IN THE ARSIA MONS FAN-SHAPED DEPOSIT, MARS.  46th Lunar and Planetary Science Conference.  2266.pdf</ref>
-<ref name="ReferenceA">{{cite journal | last1= Shean | first1= David E. | last2= Head | first2= James W. | last3= Fastook | first3= James L. | last4= Marchant | first4= David R. | title= Recent glaciation at high elevations on Arsia Mons, Mars: Implications for the formation and evolution of large tropical mountain glaciers| page= E03004 | date= 2007 | issue= E3 | volume= 112 | doi = 10.1029/2006JE002761 | journal= Journal of Geophysical Research | url=http://www.planetary.brown.edu/pdfs/3281.pdf | bibcode=2007JGRE..11203004S}}</ref> [[Pavonis Mons]],<ref name="SheanPavonis" /> and [[Olympus Mons]].<ref name="Basilevsky, A. 2006">{{Cite journal|author=Basilevsky, A.  |date=2006 |title=Geological recent tectonic, volcanic and fluvial activity on the eastern flank of the Olympus Mons volcano, Mars |journal=Geophysical Research Letters |volume=33 |issue=13 |pages=13201, L13201 |doi=10.1029/2006GL026396 |bibcode = 2006GeoRL..3313201B |last2=Werner |first2=S. C.|author2-link= Stephanie C. Werner |last3=Neukum |first3=G. |last4=Head |first4=J. W. |last5=Van Gasselt |first5=S. |last6=Gwinner |first6=K. |last7=Ivanov |first7=B. A. }}</ref>
-Scientists see evidence that [[glaciers]] exist on many of the volcanoes in Tharsis, including Olympus Mons, Ascraeus Mons, and Pavonis Mons.<ref>http://www.lpi.edu/meetings/polar2003/pdf/8105.pdf{{dead link|date=October 2017 |bot=InternetArchiveBot |fix-attempted=yes }}</ref><ref name="SheanPavonis" />  Ceraunius Tholus may have even had its glaciers melt to form some temporary lakes in the past.<ref>{{cite journal | last1=Fassett | first1=C | last2=Headiii | first2=J | title=Valley formation on martian volcanoes in the Hesperian: Evidence for melting of summit snowpack, caldera lake formation, drainage and erosion on Ceraunius Tholus | url=http://www.planetary.brown.edu/pdfs/3408.pdf | journal=Icarus | volume=189 | issue=1 | pages=118–135 | year=2007| doi = 10.1016/j.icarus.2006.12.021 | bibcode=2007Icar..189..118F}}</ref><ref>http://www.mars.asu/christensen/advancedmarsclass/shean_glaciers_2005.pdf{{dead link|date=October 2017 |bot=InternetArchiveBot |fix-attempted=yes }}</ref><ref name="Head, J. 2005"/><ref>http://www.marstoday.com/news/viewpr.html?pid=18050{{dead link|date=January 2017 |bot=InternetArchiveBot |fix-attempted=yes }}</ref><ref>http://news.brown.edu/pressreleases/2008/04/martian-glaciers</ref><ref>{{cite journal | last1= Plaut | first1= Jeffrey J. | last2= Safaeinili | first2= Ali | last3= Holt | first3= John W. | last4= Phillips | first4= Roger J. | last5= Head | first5= James W. | last6= Seu | first6= Roberto | last7= Putzig | first7= Nathaniel E. | last8= Frigeri | first8= Alessandro | title= Radar Evidence for Ice in Lobate Debris Aprons in the Mid-Northern Latitudes of Mars | journal= Geophysical Research Letters | volume= 36 | issue= 2 | pages=  n/a| year= 2009 | doi = 10.1029/2008GL036379 |url=http://www.lpi.usra.edu/meetings/lpsc2008/pdf/2290.pdf | bibcode=2009GeoRL..3602203P}}</ref><ref>{{cite journal | title= Radar Sounding Evidence for Ice within Lobate Debris Aprons near Hellas Basin, Mid-Southern Latitudes of Mars | bibcode = 2008LPI....39.2441H | url=http://www.lpi.usra.edu/meetings/lpsc2008/pdf/2441.pdf | journal = Lunar and Planetary Science |volume=XXXIX | issue = 1391 | pages = 2441 |year=2008 |last1= Holt | first=J.W.| last2 = Safaeinili | first2 = A. | last3 = Plaut | first3 = J. J. | last4 = Young | first4 = D. A. | last5 = Head | first5 = J. W. | last6 = Phillips | first6 = R. J. | last7 = Campbell | first7 = B. A. | last8 = Carter | first8 = L. M. | last9 = Gim | first9 = Y. | last10 = Seu | first10 = R. | author11 = Sharad Team }}</ref>
 ==Ice sheet==
 {{main|Dorsa Argentea Formation}}
-There is much evidence for a large ice sheet that existed in the south polar region of the planet.<ref>{{cite journal | last1 = Allen | first1 = C | year = 1979 | title = Volcano-ice interactions on Mars | url = | journal = J. Geophys. Res.: Solid Earth (1978–2012) | volume = 84 | issue = B14| pages = 8048–8059 | doi = 10.1029/jb084ib14p08048 | bibcode = 1979JGR....84.8048A }}</ref><ref>Howard, 1981</ref><ref>{{cite journal | last1 = Kargel | first1 = J. | last2 = Strom | first2 = R. | year = 1992 | title = Ancient glaciation on mars | url = | journal = Geology | volume = 20 | issue = 1| pages = 3–7 | bibcode = 1992Geo....20....3K | doi = 10.1130/0091-7613(1992)020<0003:AGOM>2.3.CO;2 }}</ref><ref>Head, J, S. Pratt.  2001.  Extensive Hesperian-aged south polar ice sheet on Mars: Evidence for massive melting and retreat, and lateral flow and pending of meltwater.  J. Geophys. Res.-Planet, 106 (E6), 12275-12299.</ref>  A large number of [[eskers]] which form under ice are found there.  The field of eskers make up the [[Dorsa Argentea Formation]].  The ice sheet had an area twice that of the state of [[Texas]].<ref>{{cite journal | last1 = Scanlon | first1 = K. |display-authors=etal | year = 2018 | title =  The Dorsa Argentea Formation and the Noachian-Hesperian climate transition| url = | journal = Icarus | volume = 299 | issue = | pages = 339–363 | bibcode = 2018Icar..299..339S| doi = 10.1016/j.icarus.2017.07.031}}</ref>
+There is much evidence for a large ice sheet that existed in the south polar region of the planet.<ref>{{cite journal | last1 = Allen | first1 = C | year = 1979 | title = Volcano-ice interactions on Mars | journal =  Journal of Geophysical Research| volume = 84 | issue = B14| pages = 8048–8059 | doi = 10.1029/jb084ib14p08048 | bibcode = 1979JGR....84.8048A }}</ref><ref>Howard, 1981</ref><ref>{{cite journal | last1 = Kargel | first1 = J. | last2 = Strom | first2 = R. | year = 1992 | title = Ancient glaciation on mars | journal = Geology | volume = 20 | issue = 1| pages = 3–7 | bibcode = 1992Geo....20....3K | doi = 10.1130/0091-7613(1992)020<0003:AGOM>2.3.CO;2 }}</ref><ref>Head, J, S. Pratt.  2001.  Extensive Hesperian-aged south polar ice sheet on Mars: Evidence for massive melting and retreat, and lateral flow and pending of meltwater.  J. Geophys. Res.-Planet, 106 (E6), 12275-12299.</ref>  A large number of [[eskers]] which form under ice are found there.  The field of eskers make up the [[Dorsa Argentea Formation]].  The ice sheet had an area twice that of the state of [[Texas]].<ref>{{cite journal | last1 = Scanlon | first1 = K. |display-authors=etal | year = 2018 | title =  The Dorsa Argentea Formation and the Noachian-Hesperian climate transition| journal = Icarus | volume = 299 | pages = 339–363 | bibcode = 2018Icar..299..339S| doi = 10.1016/j.icarus.2017.07.031}}</ref>
+Evidence also is building up for the past existence of an ice sheet in the Tharsis region.<ref>{{cite journal | doi=10.1016/j.icarus.2021.114332 | title=Landform evolution of Oudemans crater and its bounding plateau plains on Mars: Geomorphological constraints on the Tharsis ice-cap hypothesis | date=2021 | last1=Yin | first1=An | last2=Moon | first2=Seulgi | last3=Day | first3=Mackenzie | journal=Icarus | volume=360 | bibcode=2021Icar..36014332Y | doi-access=free }}</ref> <ref>Lin, A., et al.  2023.  Landform evolution of Oudemans crater and its bounding plateau plains on Mars: Geomorphological constraints on the Tharsis ice-cap hypothesis.  Icarus.  Volume 360, 15 May 2021, 114332</ref> <ref>V.R. Baker, R.G. Strom, J.M. Dohm, V.C. Gulick, J.S. Kargel, G. Komatsu, G.G. Ori, J.W. Rice Jr.  Mars’ Oceanus Borealis, ancient glaciers, and the MEGAOUTFLO hypothesis.
+Lunar Planet. Sci, XXXI (2000), p. 1863</ref> <ref>K.P. Harrison, R.E. Grimm.  2004.  Tharsis recharge: A source of groundwater for Martian outflow channels.  Geophys. Res. Lett., 31 (14) </ref> <ref> J.P. Cassanelli, J.W. Head.  2019.
+Glaciovolcanism in the Tharsis volcanic province of Mars: Implications for regional geology and hydrology.  Planet. Space Sci., 169. pp. 45-69</ref>  It would have been in the Late Hesperian time period.  When it melted it may have helped to form a northern ocean.<ref>B.K. Lucchitta
+Antarctic ice streams and outflow channels on Mars
+Geophys. Res. Lett., 28 (3) (2001), pp. 403-406</ref> <ref>M.H. Carr, J.W. Head III.  2010.  Geologic history of Mars Earth Planet. Sci. Lett., 294 (3–4). pp. 185-203</ref> <ref>M.H. Carr, J.W. Head.  2015.  Martian surface/near-surface water inventory: Sources, sinks, and changes with time
+Geophys. Res. Lett., 42 (3). pp. 726-732</ref> <ref>M. Carr, J. Head.  2019.  Mars: Formation and fate of a frozen Hesperian ocean.  Icarus, 319. pp. 433-443</ref>
 <gallery class="center" widths="190px" heights="180px" >
@@ Line 132: / Line 146: @@
 ==Ground ice==
 [[File:Mars exposed subsurface ice.jpg|thumb|A cross-section of underground water ice is exposed at the steep slope that appears bright blue in this enhanced-color view from the [[Mars Reconnaissance Orbiter|MRO]].<ref name='exposed ice 2018'>[https://www.jpl.nasa.gov/news/news.php?feature=7038 Steep Slopes on Mars Reveal Structure of Buried Ice]. NASA Press Release. 11 January 2018.</ref> The scene is about 500 meters wide. The scarp drops about 128 meters from the level ground, The ice sheets extend from just below the surface to a depth of 100 meters or more<ref>{{cite journal | doi = 10.1126/science.aao1619 | volume=359 | title=Exposed subsurface ice sheets in the Martian mid-latitudes | year=2018 | journal=Science | pages=199–201 | last1 = Dundas | first1 = Colin M. | last2 = Bramson | first2 = Ali M. | last3 = Ojha | first3 = Lujendra | last4 = Wray | first4 = James J. | last5 = Mellon | first5 = Michael T. | last6 = Byrne | first6 = Shane | last7 = McEwen | first7 = Alfred S. | last8 = Putzig | first8 = Nathaniel E. | last9 = Viola | first9 = Donna | last10 = Sutton | first10 = Sarah | last11 = Clark | first11 = Erin | last12 = Holt | first12 = John W. | issue=6372 | pmid = 29326269 | bibcode = 2018Sci...359..199D| doi-access = free }}</ref>]]
-Mars has vast glaciers hidden under a layer of rocky debris over wide areas in the mid-latitudes.  These glaciers could be large reservoir of life-supporting water on the planet for simple life forms and for future colonists.<ref>http://www.uahirise.org/ESP_049028_2065</ref> Research by John Holt, of the University of Texas at Austin, and others found that one of the features examined is three times larger than the city of Los Angeles and up to 800&nbsp;m thick, and there are many more.<ref>.http://www.timesonline.co.uk/tol/news/science/article5200977.ec</ref><ref>[http://www.nbcnews.com/id/27827606 NBC News]</ref>
+Mars has vast glaciers hidden under a layer of rocky debris over wide areas in the mid-latitudes.  These glaciers could be large reservoir of life-supporting water on the planet for simple life forms and for future colonists.<ref>{{Cite web|url=http://www.uahirise.org/ESP_049028_2065|title=HiRISE &#124; Icy Flow in a Crater (ESP_049028_2065)}}</ref> Research by John Holt, of the University of Texas at Austin, and others found that one of the features examined is three times larger than the city of Los Angeles and up to 800&nbsp;m thick, and there are many more.<ref>[http://www.timesonline.co.uk/tol/news/science/article5200977.ec The Times]{{dead link|date=September 2024|bot=medic}}{{cbignore|bot=medic}} </ref><ref>[http://www.nbcnews.com/id/27827606 NBC News]{{dead link|date=August 2024|bot=medic}}{{cbignore|bot=medic}}</ref>
 Some of the glacial-like features were revealed by NASA's Viking orbiters in the 1970s.  Since that time glacial-like features have been studied by more and more advanced instruments.  Much better data has been received from [[Mars Global Surveyor]], [[Mars Odyssey]], [[Mars Express]], and [[Mars Reconnaissance Orbiter]].
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 ==See also==
 {{div col|colwidth=30em}}
+* [[Areography (geography of Mars)]]
 * [[Climate of Mars]]
 * [[Deuteronilus Mensae]]
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 {{Geography of Mars}}
+{{Glaciers}}
 {{Portal bar|Astronomy|Solar System|Science}}