Difference between revisions of "Argyre quadrangle"

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File:Argyre region on Mars by the Viking 1 orbiter.jpg
 
File:Argyre region on Mars by the Viking 1 orbiter.jpg
 
</gallery>The Argyre quadrangle holds the Argyre basin,  a giant impact that occurred 70 million years after the Hellas impact and may have contained a lake in the early history of Mars.
 
</gallery>The Argyre quadrangle holds the Argyre basin,  a giant impact that occurred 70 million years after the Hellas impact and may have contained a lake in the early history of Mars.
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One of the biggest impact basins on Mars is in the Argyre  quadrangle.  The Argyre quadrangle covers the area from 30° to 65° south latitude and  0° to 60° west longitude 300 -360 E.  It contains [[Galle  Crater]], which resembles a smiley face.  It contains a region on Mars called [[Argyre Planitia]] and part of another called [[Noachis Terra]].  Noachis is named after Noah in the Bible.  This region contains several features that are evidence for ice in the ground.  Also, several types of landscapes are very beautiful.  These are all discussed and displayed below.
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==Name==
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The word Argyre is named after a legendary silver deposit at the mouth of the Ganges--[Arakan, Berma.<ref>Blunck, J.  1982.  Mars and its Satellites.  Exposition Press.  Smithtown, N.Y.</ref>
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Research published in the journal ''[[Icarus (journal)|Icarus]]'' has found pits in Hale Crater that are caused by hot ejecta falling on ground containing ice.  The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.<ref>{{cite journal | last1 = Tornabene | first1 = L. |display-authors=et al | year = 2012 | title = Widespread crater-related pitted materials on Mars. Further evidence for the role of target volatiles during the impact process | url = | journal = Icarus | volume = 220 | issue = 2| pages = 348–368 | doi=10.1016/j.icarus.2012.05.022 | bibcode=2012Icar..220..348T}}</ref>
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Many steep slopes in this quadrangle contain gullies, which are believed to have formed by relatively recent flows of water.
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==Argyre basin==
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The real big feature of the Argyre quadrangle is the Argyre basin, called Argyre Planitia in the geological language of Mars.  It  was  formed  by a giant impact that occurred 70 million years after the Hellas impact, the other giant impact in the Southern hemisphere.  <ref>Robbins |display-authors=et al | year = 2013 | title = large impact crater histories of Mars: The effect of different model crater age techniques | url = | journal = Icarus | volume = 225 | issue = 1| pages = 173–184 | doi=10.1016/j.icarus.2013.03.019 |</ref>  It contained a lake early in the history of Mars.<ref>Parker, T. et al. 2000.  Argyre Planitia and the Mars global hydrolocia cycle.  LPSC XXXI.  Abstract 2033</ref> At least three river valleys (Surius Vallis, Dzigal Vallis, and Palacopus Vallis) drain into it from the south.  As soon as water entered the basin, it began to freeze.  After it froze solid, the ice formed eskers which are still visible today.<ref>Kargel, J. and R. Strom.  1991.  Terrestrial glacial eskers:  analogs for martian sinuous ridges.  LPSC XXII, 683-684.</ref> <ref>Michael H. Carr|title=The surface of Mars|url=https://books.google.com/books?id=uLHlJ6sjohwC|accessdate=21 March 2011|year=2006|publisher=Cambridge University Press|</ref> Eskers are formed from streams moving under glaciers.  Many researchers argue that the impact that formed the Argyre basin probably stuck an ice cap or a thick permafrost layer.  That great impact melted the ice and formed a giant lake that eventually sent water to the North.  The lake's volume was equal to the Mediterranean Sea.  The deepest part of the lake may have taken more than a hundred thousand years to freeze, but with the help of heat from the impact, geothermal heating, and dissolved salts, it may have had liquid water for many millions of years.  Life may have developed in this time.  This region shows a great deal of evidence of glacial activity with flow features, crevasse-like fractures, drumlines, eskers, tarns, aretes, cirques, Glacial horns, U-shaped valleys, and terraces.  Because of the shapes of winding ridges called Argyre sinuous ridges, they are accepted to be  eskers.<ref>Dohm | first1 = J. | last2 = Hare | first2 = T. | last3 = Robbins | first3 = S. | last4 = Williams | first4 = J.-P. | last5 = Soare | first5 = R. | last6 = El-Maarry | first6 = M. | last7 = Conway | first7 = S. | last8 = Buczkowski | first8 = D. | last9 = Kargel | first9 = J. | last10 = Banks | first10 = M. | last11 = Fairén | first11 = A. | last12 = Schulze-Makuch | first12 = D. | last13 = Komatsu | first13 = G. | last14 = Miyamoto | first14 = H. | last15 = Anderson | first15 = R. | last16 = Davila | first16 = A. | last17 = Mahaney | first17 = W. | last18 = Fink | first18 = W. | last19 = Cleaves | first19 = H. | last20 = Yan | first20 = J. | last21 = Hynek | first21 = B. | last22 = Maruyama | first22 = S. | year = 2015 | title = Geological and hydrological histories of the Argyre province, Mars | url = | journal = Icarus | volume = 253 | issue = | pages = 66–98 | doi=10.1016/j.icarus.2015.02.017 | </ref>  <ref>Banks | first1 = M. | last2 = Lang | first2 = N. | last3 = Kargel | first3 = J. | last4 = McEwen | first4 = A. | last5 = Baker | first5 = V. | last6 = Grant | first6 = J. | last7 = Pelletier | first7 = J. | last8 = Strom | first8 = R. | year = 2009 | title = An analysis of sinuous ridges in the southern Argyre Planitia, Mars using HiRISE and CTX images and MOLA data | doi = 10.1029/2008JE003244 | journal = J. Geophys. Res. | volume =  114| issue = E9| pages = E09003 | </ref> <ref> Bernhardt | first1 = H. | last2 = Hiesinger | first2 = H. | last3 = Reiss | first3 = D. | last4 = Ivanov | first4 = M. | last5 = Erkeling | first5 = G. | year = 2013 | title = Putative eskers and new insights into glacio-fluvial depositional settings southern Argyre Planitia, Mars | url = | journal = Planet. Space Sci. | volume = 85 | issue = | pages = 261–278 | doi=10.1016/j.pss.2013.06.022 | </ref>
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<gallery class="center" widths="190px" heights="180px" >
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Image:Argyre MOLA zoom 64.jpg|Topography of the Argyre basin, the major feature in the Argyre quadrangle.
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</gallery>
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==[[Martian gullies]]==
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Gullies are common in some latitude bands on Mars—usually in midlatitudes...  Most Martian gullies are found on the walls of craters or troughs, but Charitum Montes, a group of mountains, has gullies in some areas (See the image below).
 +
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Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they sometimes are on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron.  For many years, researchers thought the gullies were made by running water.  But after many more observations it was found that gullies are being formed today which cannot happen with liquid water. <ref>Dundas, C., S.
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Diniega, and A. McEwen.  2014.  LONG-TERM MONITORING OF MARTIAN GULLY ACTIVITY WITH HIRISE.  45th Lunar and Planetary Science Conference.  2204.pdf</ref> <ref>NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm </ref> The weather conditions on present day Mars are such that sufficient liquid water cannot exist to cause gullies to form.  Experiments on the Earth showed that gullies can be made with the movement of chunks of dry ice moving down steep slope. <ref>http://spaceref.com/mars/frosty-gullies-on-mars.html</ref> Changes in gullies were seen on Mars when the temperature was just right for such movements of dry ice. <ref>Dundas, C., S. Diniega, A. McEwen. 2015. Long-term monitoring of martian gully formation and evolution with MRO/HiRISE. Icarus: 251, 244–263</ref> <ref> last1 = Raack | first1 = J. | display-authors = etal  | year = 2015 | title =  Present-day seasonal gully activity in a south polar pit (Sisyphi Cavi) on Mars| url = | journal = Icarus | volume = 251 | issue = | pages = 226–243 | doi=10.1016/j.icarus.2014.03.040 | </ref>  So, today the scientific community mostly supports the idea that gullies are forming today with dry ice moving down steep slopes. <ref name="NASA-20140710">last=Harrington |first=J.D. |last2=Webster |first2=Guy |title=RELEASE 14-191 – NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars |url=http://www.nasa.gov/press/2014/july/nasa-spacecraft-observes-further-evidence-of-dry-ice-gullies-on-mars |date=July 10, 2014 |work=NASA</ref> <ref>CNRS. "Gullies on Mars sculpted by dry ice rather than liquid water." ScienceDaily. ScienceDaily, 22 December 2015. www.sciencedaily.com/releases/2015/12/151222082255.htm </ref> <ref>http://www.skyandtelescope.com/astronomy-news/martian-gullies-triggered-by-exploding-dry-ice-122320158</ref> However, some concede that liquid water may have been involved in the past. <ref>Dundas, C., S. Diniega, C. Hansen, S. Byrne, A. McEwen.  2012.  Seasonal activity and morphological changes in martian gullies.  Icarus, 220.  124–143.</ref>
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==Layers==
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Some locations in the Argye quadrangle show layers.  Many places on Mars show such layers.<ref> Edgett | first1 = Kenneth S. | journal = The Mars Journal | volume = 1 | pages = 5–58|bibcode = 2005IJMSE...1....5E }}</ref> <ref> Malin | first1 = M. P. | last2 = Edgett | first2 = K. S. | date = 2000 | title = Ancient sedimentary rocks of early Mars | url = | journal = Science | volume = 290 | issue = 5498| pages = 1927–1937 | doi = 10.1126/science.290.5498.1927 | pmid = 11110654 |</ref>  Finding layered rocks is significant because layered materials usually need water to form.  On the Earth most layers have formed under lakes, seas, and oceans.  Martian climate changes probably helped greatly in the formation of these layers.  These climate variations are due to the tilt of the planet’s  rotational axis.  Because of these variations of climate, at times the atmosphere of Mars would have been much thicker and contained more moisture.  The amount of atmospheric dust also has increased and decreased. It is believed that these frequent changes helped to deposit material in craters and other low places. The rising of mineral-rich ground water cemented these materials. Layers may be formed by groundwater rising up depositing minerals and cementing sediments.  The hardened layers are consequently more protected from erosion.  This process may occur instead of layers forming under lakes.
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<gallery class="center" widths="190px" heights="180px" >
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ESP 042597 1320layers.jpg|Layers exposed in [[Nereidum Montes]], as seen by HiRISE under HiWish program  The light-toned layers may contain sulfates which are good for preserving traces of ancient life.
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42597 1320layers2.jpg|Close-up of layers from previous image, as seen by HiRISE under HiWish program
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ESP 043413 1495layers.jpg|Low, layered mesa, as seen by HiRISE under HiWish program  Arrows point to some layers.
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ESP 047410 1235layers.jpg|Layers, as seen by HiRISE under HiWish program
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</gallery>
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<gallery class="center" widths="190px" heights="180px" >
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ESP 048003 1495layers.jpg|Wide view of crater showing layers along wall, as seen by HiRISE under HiWish program
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48003 1495layerslight.jpg|Close view of layers in crater wall,  as seen by HiRISE under HiWish program
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48003 1495cratermesa.jpg|Layers in mesa on floor of crater,  as seen by HiRISE under HiWish program
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</gallery>
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==Channels==
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This region, as many other regions on Mars shows evidence of water in the past.  Well-formed channels are present.  There is enormous evidence that water once flowed in river valleys on Mars.<ref>Baker, V., et al.  2015.  Fluvial geomorphology on Earth-like planetary surfaces: a review.  Geomorphology.  245, 149–182.</ref><ref>Carr, M.  1996.  in Water on Mars.  Oxford Univ. Press.</ref>  Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the [[Mariner 9]] orbiter.<ref>Baker, V.  1982.  The Channels of Mars. Univ. of Tex. Press, Austin, TX</ref><ref>Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale.  1991.  Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.</ref> <ref>Carr, M.  1979.  Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.</ref> <ref>Komar, P.  1979.  Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.</ref>  The volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had.  Water was probably recycled many times from the ocean to rainfall around Mars.<ref>http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html</ref> <ref>Luo, W., et al.  2017.  New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate.  Nature Communications 8.  Article number:  15766 (2017).  doi:10.1038/ncomms15766</ref>  The climate of Mars may have been such in the past that water may have ran on its surface.  It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as our moon stabilizes Earth; at times the tilt of Mars has even been greater than 80 degrees<ref> Touma J. and J. Wisdom.  1993.  The Chaotic Obliquity of Mars.  Science 259, 1294-1297.</ref> <ref>Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel.  2004.  Long term evolution and chaotic diffusion of the insolation quantities of Mars.  Icarus 170, 343-364.</ref>
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<gallery class="center" widths="190px" heights="180px" >
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ESP 047265 1415channel.jpg|Channel, as seen by HiRISE under HiWish program
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ESP 048043 1460channel.jpg|Channel, as seen by HiRISE under HiWish program
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Image:Surface features in Argyre.jpg|Channels in Argyre quadrangle as seen by HiRISE, under the HiWish program.  This is the image of the surface from a single HiRISE image.  The scale bar at the top is 500 meters long.
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ESP 050243 1425channel.jpg|Channel, as seen by HiRISE under HiWish program
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</gallery>
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==Dust devil tracks==
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Dust devil tracks can be very pretty.  They are caused by giant dust devils removing bright colored dust from the Martian surface; thereby exposing a dark layer.  Dust devils on Mars have been photographed both from the ground and high overhead from orbit. They have even blown dust off the solar panels of two Rovers on Mars, thereby greatly extending their useful lifetime.<ref>http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412</ref> The pattern of the tracks has been shown to change every few months.<ref>http://hirise.lpl.arizona.edu/PSP_005383_1255</ref>  A study that combined data from the High Resolution Stereo Camera (HRSC) and the Mars Orbiter Camera (MOC) found that some large dust devils on Mars have a diameter of 700 m and last at least 26 minutes.<ref>Reiss, D. et al.  2011.  Multitemporal observations of identical active dust devils on Mars with High Resolution Stereo Camera (HRSC) and Mars Orbiter Camera (MOC).  Icarus.  215:358-369.</ref>
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<gallery class="center" widths="190px" heights="180px" >
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ESP 048583 1260devilslayers.jpg|Dust devil tracks and layers, as seen by HiRISE under HiWish program
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ESP 048583 1260devilsclosecolor.jpg|Close, color view of dust devil tracks, as seen by HiRISE under HiWish program
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ESP 039919 1375devils.jpg|[[Dust devil tracks]] as seen by HiRISE under HiWish program
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</gallery>
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==Dunes==
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<gallery class="center" widths="190px" heights="180px" >
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File:ESP 057445 1385dunes.jpg|Wide view of small dune field, as seen by HiRISE under HiWish program
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File:57445 1385dunesclose.jpg|Close view of dunes, as seen by HiRISE under HiWish program  Ripples are visible on the dunes.
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</gallery>
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== Other features in Argyre quadrangle==
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<gallery class="center" widths="190px" heights="180px" >
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ESP 048280 1395hollows.jpg|Hollows, as seen by HiRISE under HiWish program
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File:ESP 054570 1465pingos.jpg|Possible pingos, as seen by HiRISE under HiWish program  Pingos contain a core of ice.  They are expected to have cracks on their surfaces because water expands when it turns into ice.
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</gallery>
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<gallery class="center" widths="190px" heights="180px" >
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File:ESP 055453 1250iceintroughs.jpg|Wide view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program
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File:55453 1250icetroughs.jpg|Close view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program
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File:55453 1250polygonsice.jpg|Close view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program
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</gallery>
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<gallery class="center" widths="190px" heights="180px" >
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ESP 048583 1260devilslayers.jpg|Dust devil tracks and layers, as seen by HiRISE under HiWish program
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ESP 048583 1260devilsclosecolor.jpg|Close, color view of dust devil tracks, as seen by HiRISE under HiWish program
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ESP 039919 1375devils.jpg|[[Dust devil tracks]] as seen by HiRISE under HiWish program
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File:ESP 057669 1245devils.jpg|Dust devil tracks, as seen by HiRISE under HiWish program
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</gallery>
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[[Category:  Mars Atlas]]
 
[[Category:  Mars Atlas]]

Revision as of 11:49, 1 March 2020

Mars topography (MOLA dataset) HiRes (1).jpg
MC-26 Argyre 30–65° S 0–60° W Quadrangles Atlas
  • USGS-Mars-MC-26-ArgyreRegion-mola.png
  • Argyre region on Mars by the Viking 1 orbiter.jpg

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


One of the biggest impact basins on Mars is in the Argyre quadrangle. The Argyre quadrangle covers the area from 30° to 65° south latitude and 0° to 60° west longitude 300 -360 E. It contains Galle Crater, which resembles a smiley face. It contains a region on Mars called Argyre Planitia and part of another called Noachis Terra. Noachis is named after Noah in the Bible. This region contains several features that are evidence for ice in the ground. Also, several types of landscapes are very beautiful. These are all discussed and displayed below.

Name

The word Argyre is named after a legendary silver deposit at the mouth of the Ganges--[Arakan, Berma.[1]


Research published in the journal Icarus has found pits in Hale Crater that are caused by hot ejecta falling on ground containing ice. The pits are formed by heat forming steam that rushes out from groups of pits simultaneously, thereby blowing away from the pit ejecta.[2] Many steep slopes in this quadrangle contain gullies, which are believed to have formed by relatively recent flows of water.

Argyre basin

The real big feature of the Argyre quadrangle is the Argyre basin, called Argyre Planitia in the geological language of Mars. It was formed by a giant impact that occurred 70 million years after the Hellas impact, the other giant impact in the Southern hemisphere. [3] It contained a lake early in the history of Mars.[4] At least three river valleys (Surius Vallis, Dzigal Vallis, and Palacopus Vallis) drain into it from the south. As soon as water entered the basin, it began to freeze. After it froze solid, the ice formed eskers which are still visible today.[5] [6] Eskers are formed from streams moving under glaciers. Many researchers argue that the impact that formed the Argyre basin probably stuck an ice cap or a thick permafrost layer. That great impact melted the ice and formed a giant lake that eventually sent water to the North. The lake's volume was equal to the Mediterranean Sea. The deepest part of the lake may have taken more than a hundred thousand years to freeze, but with the help of heat from the impact, geothermal heating, and dissolved salts, it may have had liquid water for many millions of years. Life may have developed in this time. This region shows a great deal of evidence of glacial activity with flow features, crevasse-like fractures, drumlines, eskers, tarns, aretes, cirques, Glacial horns, U-shaped valleys, and terraces. Because of the shapes of winding ridges called Argyre sinuous ridges, they are accepted to be eskers.[7] [8] [9]

  • Topography of the Argyre basin, the major feature in the Argyre quadrangle.

Martian gullies

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

Gullies occur on steep slopes, especially on the walls of craters. Gullies are believed to be relatively young because they have few, if any craters. Moreover, they sometimes are on top of sand dunes which themselves are considered to be quite young. Usually, each gully has an alcove, channel, and apron. For many years, researchers thought the gullies were made by running water. But after many more observations it was found that gullies are being formed today which cannot happen with liquid water. [10] [11] The weather conditions on present day Mars are such that sufficient liquid water cannot exist to cause gullies to form. Experiments on the Earth showed that gullies can be made with the movement of chunks of dry ice moving down steep slope. [12] Changes in gullies were seen on Mars when the temperature was just right for such movements of dry ice. [13] [14] So, today the scientific community mostly supports the idea that gullies are forming today with dry ice moving down steep slopes. [15] [16] [17] However, some concede that liquid water may have been involved in the past. [18]

Layers

Some locations in the Argye quadrangle show layers. Many places on Mars show such layers.[19] [20] Finding layered rocks is significant because layered materials usually need water to form. On the Earth most layers have formed under lakes, seas, and oceans. Martian climate changes probably helped greatly in the formation of these layers. These climate variations are due to the tilt of the planet’s rotational axis. Because of these variations of climate, at times the atmosphere of Mars would have been much thicker and contained more moisture. The amount of atmospheric dust also has increased and decreased. It is believed that these frequent changes helped to deposit material in craters and other low places. The rising of mineral-rich ground water cemented these materials. Layers may be formed by groundwater rising up depositing minerals and cementing sediments. The hardened layers are consequently more protected from erosion. This process may occur instead of layers forming under lakes.

  • Layers exposed in Nereidum Montes, as seen by HiRISE under HiWish program The light-toned layers may contain sulfates which are good for preserving traces of ancient life.

  • Close-up of layers from previous image, as seen by HiRISE under HiWish program

  • Low, layered mesa, as seen by HiRISE under HiWish program Arrows point to some layers.

  • Layers, as seen by HiRISE under HiWish program

  • Wide view of crater showing layers along wall, as seen by HiRISE under HiWish program

  • Close view of layers in crater wall, as seen by HiRISE under HiWish program

  • Layers in mesa on floor of crater, as seen by HiRISE under HiWish program

Channels

This region, as many other regions on Mars shows evidence of water in the past. Well-formed channels are present. There is enormous evidence that water once flowed in river valleys on Mars.[21][22] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[23][24] [25] [26] The volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.[27] [28] The climate of Mars may have been such in the past that water may have ran on its surface. It has been known for some time that Mars undergoes many large changes in its tilt or obliquity because its two small moons lack the gravity to stabilize it, as our moon stabilizes Earth; at times the tilt of Mars has even been greater than 80 degrees[29] [30]

  • Channel, as seen by HiRISE under HiWish program

  • Channel, as seen by HiRISE under HiWish program

  • Channels in Argyre quadrangle as seen by HiRISE, under the HiWish program. This is the image of the surface from a single HiRISE image. The scale bar at the top is 500 meters long.

  • Channel, as seen by HiRISE under HiWish program

Dust devil tracks

Dust devil tracks can be very pretty. They are caused by giant dust devils removing bright colored dust from the Martian surface; thereby exposing a dark layer. Dust devils on Mars have been photographed both from the ground and high overhead from orbit. They have even blown dust off the solar panels of two Rovers on Mars, thereby greatly extending their useful lifetime.[31] The pattern of the tracks has been shown to change every few months.[32] A study that combined data from the High Resolution Stereo Camera (HRSC) and the Mars Orbiter Camera (MOC) found that some large dust devils on Mars have a diameter of 700 m and last at least 26 minutes.[33]

  • Dust devil tracks and layers, as seen by HiRISE under HiWish program

  • Close, color view of dust devil tracks, as seen by HiRISE under HiWish program

  • Dust devil tracks as seen by HiRISE under HiWish program

Dunes

  • Wide view of small dune field, as seen by HiRISE under HiWish program

  • Close view of dunes, as seen by HiRISE under HiWish program Ripples are visible on the dunes.

Other features in Argyre quadrangle

  • Hollows, as seen by HiRISE under HiWish program

  • Possible pingos, as seen by HiRISE under HiWish program Pingos contain a core of ice. They are expected to have cracks on their surfaces because water expands when it turns into ice.

  • Wide view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program

  • Close view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program

  • Close view of polygons with ice in troughs between polygons, as seen by HiRISE under HiWish program


  • Dust devil tracks and layers, as seen by HiRISE under HiWish program

  • Close, color view of dust devil tracks, as seen by HiRISE under HiWish program

  • Dust devil tracks as seen by HiRISE under HiWish program

  • Dust devil tracks, as seen by HiRISE under HiWish program

  1. ↑ Blunck, J. 1982. Mars and its Satellites. Exposition Press. Smithtown, N.Y.
  2. ↑ "Widespread crater-related pitted materials on Mars. Further evidence for the role of target volatiles during the impact process" (2012). Icarus 220 (2): 348–368. doi:10.1016/j.icarus.2012.05.022. Bibcode: 2012Icar..220..348T. 
  3. ↑ Robbins |display-authors=et al | year = 2013 | title = large impact crater histories of Mars: The effect of different model crater age techniques | url = | journal = Icarus | volume = 225 | issue = 1| pages = 173–184 | doi=10.1016/j.icarus.2013.03.019 |
  4. ↑ Parker, T. et al. 2000. Argyre Planitia and the Mars global hydrolocia cycle. LPSC XXXI. Abstract 2033
  5. ↑ Kargel, J. and R. Strom. 1991. Terrestrial glacial eskers: analogs for martian sinuous ridges. LPSC XXII, 683-684.
  6. ↑ Michael H. Carr|title=The surface of Mars|url=https://books.google.com/books?id=uLHlJ6sjohwC%7Caccessdate=21 March 2011|year=2006|publisher=Cambridge University Press|
  7. ↑ Dohm | first1 = J. | last2 = Hare | first2 = T. | last3 = Robbins | first3 = S. | last4 = Williams | first4 = J.-P. | last5 = Soare | first5 = R. | last6 = El-Maarry | first6 = M. | last7 = Conway | first7 = S. | last8 = Buczkowski | first8 = D. | last9 = Kargel | first9 = J. | last10 = Banks | first10 = M. | last11 = Fairén | first11 = A. | last12 = Schulze-Makuch | first12 = D. | last13 = Komatsu | first13 = G. | last14 = Miyamoto | first14 = H. | last15 = Anderson | first15 = R. | last16 = Davila | first16 = A. | last17 = Mahaney | first17 = W. | last18 = Fink | first18 = W. | last19 = Cleaves | first19 = H. | last20 = Yan | first20 = J. | last21 = Hynek | first21 = B. | last22 = Maruyama | first22 = S. | year = 2015 | title = Geological and hydrological histories of the Argyre province, Mars | url = | journal = Icarus | volume = 253 | issue = | pages = 66–98 | doi=10.1016/j.icarus.2015.02.017 |
  8. ↑ Banks | first1 = M. | last2 = Lang | first2 = N. | last3 = Kargel | first3 = J. | last4 = McEwen | first4 = A. | last5 = Baker | first5 = V. | last6 = Grant | first6 = J. | last7 = Pelletier | first7 = J. | last8 = Strom | first8 = R. | year = 2009 | title = An analysis of sinuous ridges in the southern Argyre Planitia, Mars using HiRISE and CTX images and MOLA data | doi = 10.1029/2008JE003244 | journal = J. Geophys. Res. | volume = 114| issue = E9| pages = E09003 |
  9. ↑ Bernhardt | first1 = H. | last2 = Hiesinger | first2 = H. | last3 = Reiss | first3 = D. | last4 = Ivanov | first4 = M. | last5 = Erkeling | first5 = G. | year = 2013 | title = Putative eskers and new insights into glacio-fluvial depositional settings southern Argyre Planitia, Mars | url = | journal = Planet. Space Sci. | volume = 85 | issue = | pages = 261–278 | doi=10.1016/j.pss.2013.06.022 |
  10. ↑ Dundas, C., S. Diniega, and A. McEwen. 2014. LONG-TERM MONITORING OF MARTIAN GULLY ACTIVITY WITH HIRISE. 45th Lunar and Planetary Science Conference. 2204.pdf
  11. ↑ NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm
  12. ↑ http://spaceref.com/mars/frosty-gullies-on-mars.html
  13. ↑ Dundas, C., S. Diniega, A. McEwen. 2015. Long-term monitoring of martian gully formation and evolution with MRO/HiRISE. Icarus: 251, 244–263
  14. ↑ last1 = Raack | first1 = J. | display-authors = etal | year = 2015 | title = Present-day seasonal gully activity in a south polar pit (Sisyphi Cavi) on Mars| url = | journal = Icarus | volume = 251 | issue = | pages = 226–243 | doi=10.1016/j.icarus.2014.03.040 |
  15. ↑ last=Harrington |first=J.D. |last2=Webster |first2=Guy |title=RELEASE 14-191 – NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars |url=http://www.nasa.gov/press/2014/july/nasa-spacecraft-observes-further-evidence-of-dry-ice-gullies-on-mars |date=July 10, 2014 |work=NASA
  16. ↑ CNRS. "Gullies on Mars sculpted by dry ice rather than liquid water." ScienceDaily. ScienceDaily, 22 December 2015. www.sciencedaily.com/releases/2015/12/151222082255.htm
  17. ↑ http://www.skyandtelescope.com/astronomy-news/martian-gullies-triggered-by-exploding-dry-ice-122320158
  18. ↑ Dundas, C., S. Diniega, C. Hansen, S. Byrne, A. McEwen. 2012. Seasonal activity and morphological changes in martian gullies. Icarus, 220. 124–143.
  19. ↑ Edgett | first1 = Kenneth S. | journal = The Mars Journal | volume = 1 | pages = 5–58|bibcode = 2005IJMSE...1....5E }}
  20. ↑ Malin | first1 = M. P. | last2 = Edgett | first2 = K. S. | date = 2000 | title = Ancient sedimentary rocks of early Mars | url = | journal = Science | volume = 290 | issue = 5498| pages = 1927–1937 | doi = 10.1126/science.290.5498.1927 | pmid = 11110654 |
  21. ↑ Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.
  22. ↑ Carr, M. 1996. in Water on Mars. Oxford Univ. Press.
  23. ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  24. ↑ Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
  25. ↑ Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
  26. ↑ Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
  27. ↑ http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html
  28. ↑ Luo, W., et al. 2017. New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate. Nature Communications 8. Article number: 15766 (2017). doi:10.1038/ncomms15766
  29. ↑ Touma J. and J. Wisdom. 1993. The Chaotic Obliquity of Mars. Science 259, 1294-1297.
  30. ↑ Laskar, J., A. Correia, M. Gastineau, F. Joutel, B. Levrard, and P. Robutel. 2004. Long term evolution and chaotic diffusion of the insolation quantities of Mars. Icarus 170, 343-364.
  31. ↑ http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412
  32. ↑ http://hirise.lpl.arizona.edu/PSP_005383_1255
  33. ↑ Reiss, D. et al. 2011. Multitemporal observations of identical active dust devils on Mars with High Resolution Stereo Camera (HRSC) and Mars Orbiter Camera (MOC). Icarus. 215:358-369.
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