Scalloped topography

Scalloped topography is common in the mid-latitudes of Mars, between 45° and 60° north and south. It is particularly prominent in the region of Utopia Planitia,[1][2] in the northern hemisphere, and in the region of Peneus and Amphitrites Paterae[3][4] in the southern hemisphere. Such topography consists of shallow, rimless depressions with scalloped edges, commonly referred to as "scalloped depressions" or simply "scallops". Scalloped depressions can be isolated or clustered and sometimes seem to coalesce. A typical scalloped depression displays a gentle equator-facing slope and a steeper pole-facing scarp.[5] This topographic asymmetry is probably due to differences in insolation. Scalloped depressions are believed to form from the removal of subsurface material, possibly interstitial ice, by sublimation (direct transition of a material from the solid to the gas phase with no intermediate liquid stage). This process may still be happening at present.[6] This topography may be of great importance for future colonization of Mars because it may point to deposits of pure ice.[7]

A study published in Icarus, found that the landforms of scalloped topography can be made by the subsurface loss of water ice by sublimation under current Martian climate conditions over periods of tens of thousands of Mars years. Scalloped depressions are thought to begin with a small trigger like a small impact, local darkening, erosion, or cracks from thermal contraction. Cracks are common in ice-rich ground on the Earth. Their model predicts that these scalloped depression will develop when the ground has large amounts of pure ice, up to many tens of meters in depth. So, scalloped features can serve as markers for large deposits of pure ice. Ice in and around scalloped topography is not just in the pore spaces of the ground it is excess ice, probably 99% pure as was found by the Phoenix mission.[8][9][10] The shallow Subsurface Radar (SHARAD), aboard the Mars Reconnaissance Orbiter can detect ice-rich layers only when thicker than 10–20 meters over wide areas;[11] it has discovered ice in the region of scalloped topography.[7][12]

The details on the formation of scalloped topography still being worked out. One study, published in 2016 in Icarus proposes a five step process.

  1. Major changes in the planet’s tilt change the climate. This climate change causes an icy mantle to form.
  2. Various conditions cause the mantle to thaw or evaporate.
  3. Meltwater moves in the ground, at least to the depth of the scalloped depressions.
  4. Freezing and thawing of the ice produces masses of ice (ice lenses).
  5. With another tilt change the climate changes and masses of ice sublimate, resulting in scalloped depressions.[13]

In Utopia Planitia, a series of curvilinear ridges parallel to the scarp are etched on the floor of large scalloped depressions, possibly representing different stages of scarp erosion.[1] Recently, other researchers have advanced an idea that the ridges represent the tops of layers.[14] Sometimes the surface around scalloped terrain or scalloped topography displays "patterned ground", characterized by a regular pattern of polygonal fractures. These patterns indicate that the surface has undergone stress, perhaps caused by subsidence, desiccation, or thermal contraction.[15] Such patterns are common in periglacial areas on Earth. Scalloped terrains in Utopia Planitia display polygonal features of different sizes: small (about 5–10 m across) on the scarp, and larger (30–50 m across) on the surrounding terrains. These scale differences may indicate local difference in ground ice concentrations.[1]

Detection of underground ice

On November 22, 2016, NASA reported finding a large amount of underground ice in the Utopia Planitia region of Mars. The volume of water detected has been estimated to be equivalent to the volume of water in Lake Superior.[16][17][18]

Mars – Scalloped terrain at Utopia Planitia (November 22, 2016)
Martian terrain
Map of terrain

The calculations for the volume of water ice in the region were based on measurements from the ground-penetrating radar instrument on Mars Reconnaissance Orbiter, called SHARAD.

SHARAD finds ice by measuring its radar returns from the surface and from a deeper lower surface. The depth to the lower surface was found from HiRISE images of gaps in the surface.

From the data obtained from SHARAD, dielectric permittivity, or the dielectric constant was determined. That was found from the amount of penetration of the radar to a reflector at the bottom of the ice-rich layer. The depth to the reflector was found by examining high resolution photos of the location. Certain places had gaps or windows in the ice rich layer. MOLA topographic maps then told the depth. The top of the ice-rich layer displayed polygons, scalloped depressions, and exhuming craters all of which are believed to indicate ice.[19] At the bottom of the gap was a totally different surface of a different color and full of craters; this was the reflector seen in the radar returns. The dielectric constant, averaged over the entire area, came out to be 2.8. Solid water ice would have a dielectric of 3.0–3.2. Basalt rock which is widespread on Mars would yield 8. So using a ternary diagram from a paper by Ali Bramson et al., the researchers decided the ice-rich layer was a mixture composed of 50–80% water ice, 0–30% rocky content, and 15–50% porosity.[20][21][22]

  • Scalloped terrain at Peneus Patera, as seen by HiRISE. Scalloped terrain is quite common in some areas of Mars. Image is from the Noachis quadrangle.
    Scalloped terrain at Peneus Patera, as seen by HiRISE. Scalloped terrain is quite common in some areas of Mars. Image is from the Noachis quadrangle.
  • Periglacial forms in Utopia, as seen by HiRISE, showing patterned ground and scalloped topography. Image in Casius quadrangle.
    Periglacial forms in Utopia, as seen by HiRISE, showing patterned ground and scalloped topography. Image in Casius quadrangle.
  • Mad Vallis, as seen by HiRISE, exhibiting scalloped terrain. Picture on right is an enlargement of part of the other picture. Image in Hellas quadrangle.
    Mad Vallis, as seen by HiRISE, exhibiting scalloped terrain. Picture on right is an enlargement of part of the other picture. Image in Hellas quadrangle.
  • Scalloped ground, as seen by HiRISE under HiWish program.
    Scalloped ground, as seen by HiRISE under HiWish program.
  • Close up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.
    Close up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.
  • Scalloped ground, as seen by HiRISE under HiWish program.
    Scalloped ground, as seen by HiRISE under HiWish program.
  • Close-up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.
    Close-up of scalloped ground, as seen by HiRISE under HiWish program. Surface is divided into polygons; these forms are common where ground freezes and thaws. Note: this is an enlargement of a previous image.
  • Stages in scallop formation, as seen by HiRISE. Location is Hellas quadrangle.
    Stages in scallop formation, as seen by HiRISE. Location is Hellas quadrangle.
  • Periglacial Scallops and polygons, as seen by HiRISE under HiWish program.
    Periglacial Scallops and polygons, as seen by HiRISE under HiWish program.
  • Possible variation of scalloped terrain in depressions with straight southern walls, as seen by HiRISE under HiWish program. Box indicates part enlarged in images below. Image located in Diacria quadrangle in Milankovic crater.
    Possible variation of scalloped terrain in depressions with straight southern walls, as seen by HiRISE under HiWish program. Box indicates part enlarged in images below. Image located in Diacria quadrangle in Milankovic crater.
  • Enlargement of above image of straight walled depression, as seen by HiRISE under HiWish program. Note that the southern wall is dark compared to the northern wall.
    Enlargement of above image of straight walled depression, as seen by HiRISE under HiWish program. Note that the southern wall is dark compared to the northern wall.
  • Further enlargement of above image, as seen by HiRISE under HiWish program.
    Further enlargement of above image, as seen by HiRISE under HiWish program.
  • Low center polygons, shown with arrows, as seen by HiRISE under HiWish program Image was enlarged with HiView.
    Low center polygons, shown with arrows, as seen by HiRISE under HiWish program Image was enlarged with HiView.
  • High center polygons, shown with arrows, as seen by HiRISE under HiWish program. Image enlarged with HiView.
    High center polygons, shown with arrows, as seen by HiRISE under HiWish program. Image enlarged with HiView.
  • Scalloped terrain labeled with both low center polygons and high center polygons, as seen by HiRISE under HiWish program Image enlarged with HiView.
    Scalloped terrain labeled with both low center polygons and high center polygons, as seen by HiRISE under HiWish program Image enlarged with HiView.
  • Scalloped terrain, as seen by HiRISE under HiWish program The location is the Casius quadrangle.
    Scalloped terrain, as seen by HiRISE under HiWish program The location is the Casius quadrangle.

Interactive Mars map
Map of Mars
The image above contains clickable linksInteractive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.
(See also: Mars Rovers map and Mars Memorial map) (view • discuss)

References
  1. Lefort, A.; Russell, P.; Thomas, N.; McEwen, A.S.; Dundas, C.M.; Kirk, R.L. (2009). "HiRISE observations of periglacial landforms in Utopia Planitia". Journal of Geophysical Research. 114 (E4): E04005. Bibcode:2009JGRE..114.4005L. doi:10.1029/2008JE003264.
  2. Morgenstern A, Hauber E, Reiss D, van Gasselt S, Grosse G, Schirrmeister L (2007): Deposition and degradation of a volatile-rich layer in Utopia Planitia, and implications for climate history on Mars. Journal of Geophysical Research: Planets 112, E06010.
  3. Lefort, A.; Russell, P.; Thomas, N. (2009). "Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE". Icarus. 205 (1): 259–268. Bibcode:2010Icar..205..259L. doi:10.1016/j.icarus.2009.06.005.
  4. Zanetti, M., Hiesinger, H., Reiss, D., Hauber, E. and Neukum, G. (2009), "Scalloped Depression Development on Malea Planum and the Southern Wall of the Hellas Basin, Mars", 40th Lunar and Planetary Science Conference, abstract 2178
  5. "HiRISE | Pitted Landforms in Southern Hellas Planitia (ESP_038821_1235)".
  6. "Scalloped Topography in Peneus Patera Crater". HiRISE Operations Center. 2007-02-28. Retrieved 2014-11-24.
  7. Dundas, C.; Bryrne, S.; McEwen, A. (2015). "Modeling the development of martian sublimation thermokarst landforms". Icarus. 262: 154–169. Bibcode:2015Icar..262..154D. doi:10.1016/j.icarus.2015.07.033.
  8. Smith, P.; et al. (2009). "H2O at the Phoenix landing site". Science. 325 (5936): 58–61. Bibcode:2009Sci...325...58S. doi:10.1126/science.1172339. PMID 19574383. S2CID 206519214.
  9. Mellon, M.; et al. (2009). "Ground ice at the Phoenix landing site: Stability state and origin". J. Geophys. Res. 114 (53): E00E07. Bibcode:2009JGRE..114.0E07M. doi:10.1029/2009JE003417.
  10. Cull, S; et al. (2010). "Compositions of subsurface ices at the Mars Phoenix landing site". Geophys. Res. Lett. 37 (24): L24203. Bibcode:2010GeoRL..3724203C. doi:10.1029/2010GL045372.
  11. Seu, R.; et al. (2007). "SHARAD sounding radar on the Mars Reconnaissance Orbiter". J. Geophys. Res. 112 (E5): E05S05. Bibcode:2007JGRE..112.5S05S. doi:10.1029/2006JE002745.
  12. Stuurman, C., et al. 2016. SHARAD reflectors in Utopia Planitia, SHARAD detection and characterization of subsurface water ice deposits in Utopia Planitia, Mars. Geophysical Research Letters, Volume 43, Issue 18, 28 September 2016, Pages 9484–9491.
  13. Soare, R., et al. 2016. Ice-rich (periglacial) vs icy (glacial) depressions in the Argyre region, Mars: a proposed cold-climate dichotomy of landforms: 282, 70-83.
  14. Sejourne, A.; et al. (2012). "Evidence of an eolian ice-rich and stratified permafrost in Utopia Planitia, Mars". Icarus. 60 (1): 248–254. Bibcode:2012P&SS...60..248S. doi:10.1016/j.pss.2011.09.004.
  15. "Scalloped Depressions with Layers in the Northern Plains". HiRISE Operations Center. 2007-02-28. Retrieved 2014-11-24.
  16. Staff (November 22, 2016). "Scalloped Terrain Led to Finding of Buried Ice on Mars". NASA. Retrieved November 23, 2016.
  17. "Lake of frozen water the size of New Mexico found on Mars – NASA". The Register. November 22, 2016. Retrieved November 23, 2016.
  18. "Mars Ice Deposit Holds as Much Water as Lake Superior". NASA. November 22, 2016. Retrieved November 23, 2016.
  19. Stuurman, C., et al. 2014. "Sharad reflectors in Utopia Planitia, Mars consistent with widespread, thick subsurface ice". 45th Lunar and Planetary Science Conference.
  20. Bramson, A, et al. 2015. Widespread excess ice in Arcadia Planitia, Mars. Geophysical Research Letters: 42, 6566-6574
  21. "Widespread, Thick Water Ice found in Utopia Planitia, Mars | Cassie Stuurman". Archived from the original on 2016-11-30. Retrieved 2016-11-29.
  22. Stuurman, C., et al. 2016. SHARAD detection and characterization of subsurface water ice deposits in Utopia Planitia, Mars. Geophysical Research Letters: 43, 9484_9491.
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