Noachis quadrangle

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Mars topography (MOLA dataset) HiRes (1).jpg
MC-27 Noachis 30–65° S 0–60° E Quadrangles Atlas
  • USGS-Mars-MC-27-NoachisRegion-mola.png
  • Noachis Terra.jpg

The Noachis quadrangle covers the area from 30° to 65° south latitude and 300° to 360° west longitude (60-0 E). It lies between Argyre and Hellas, two giant impact basins on Mars. The Noachis quadrangle includes Noachis Terra and the western part of Hellas Planitia, which are classical names for regions on Mars. Noachis is considered among the oldest regions on Mars since it is so densely covered with impact craters. The oldest parts of Mars have the designation of “Noachian age." In addition, many previously buried craters are now coming to the surface.[1] Noachis' extreme age has allowed ancient craters to be filled, and once again become newly exposed. Much of the surface in Noachis quadrangle shows a scalloped topography in which the disappearance of ground ice has left depressions.[2] The first piece of human technology to land on Mars landed (crashed) in the Noachis quadrangle. It was the Soviet's Mars 2 that crash landed at 44.2 S and 313.2 W. It weighed about one ton. The automated craft attempted to land in a giant dust storm and in an area that has many dust devils.[3]

Scalloped topography

Certain regions of Mars display scalloped-shaped depressions. The depressions are believed to be the remains of an ice-rich mantle deposit. Scallops are created when ice sublimates from frozen soil.[4] [5] This mantle material probably fell from the air as ice formed on dust when the climate was different due to changes in the tilt of the Mars pole.[6] The scallops are typically tens of meters deep and from a few hundred to a few thousand meters across. They can be almost circular or elongated. Some appear to have coalesced, thereby causing a large heavily pitted terrain to form. 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. This model predicts similar shapes when the ground has large amounts of pure ice, up to many tens of meters in depth.[7] The process of producing the terrain may begin with sublimation from a crack because there are often polygon cracks where scallops form.[8] In other words, when we see this type of surface, we know there is probably ice in the ground. Future astronauts may mine this terrain for water.

  • Close view of scalloped topography, as seen by HiRISE

  • Scalloped topography, as seen by HiRISE under HiWish program

Dust Devil Tracks

Many areas on Mars experience the passage of giant dust devils. A thin coating of fine bright dust covers most of the Martian surface. When a dust devil goes by it blows away the coating and exposes the underlying dark surface creating tracks. It does not take too much fine dust to cover those tracks--experiments in Earth laboratories demonstrate that only a few 10's of microns of dust will be enough. The width of a single human hair ranges from approximately 20 to 200 microns (μm); consequently, the dust that can cover dust devil tracks may only be the thickness of a human hair.[9] Dust devils have been seen from the ground and from orbit. They have even blown the dust off of the solar panels of the two Mars Exploration Rovers (Spirit and Opportunity), thereby greatly extending their lives.[10] The twin Rovers were designed to last for 3 months, instead they lasted many years with Opportunity lasting over 14 years. The pattern of the dust devil tracks have been shown to change every few months.[11] One 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 meters and last at least 26 minutes.[12] The image below of Russel Crater shows changes in dust devil tracks over a period of only three months, as documented by HiRISE.

  • Russell Crater Dust Devil Changes, as seen by HiRISE. Click on image to see changes in dust devil tracks in just 3 months.

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

Craters

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak.[13] The peak is caused by a rebound of the crater floor following the impact.[14] Sometimes craters will display layers. Craters can show us what lies deep under the surface.

  • Close-up of layers in west slope of Asimov Crater. Shadows show the overhang. Some of the layers are much more resistant to erosion, so they stick out. Image from HiRISE.

  • Kaiser Crater (large crater in upper part of image)context for THEMIS image.

  • Detail of south wall of Kaiser Crater, as seen by THEMIS. Top of image shows part of a dune field.

  • Crater that was buried in another age and is now being exposed by erosion, as seen by the Mars Global Surveyor, under the MOC Public Targeting Program.

  • Floor of crater in Noachis quadrangle, as seen by HiRISE under HiWish program.

Sand Dunes

When there are perfect conditions for producing sand dunes, steady wind in one direction and just enough sand, a barchan sand dune forms. Barchans have a gentle slope on the wind side and a much steeper slope on the lee side where horns or a notch often forms.[15] One picture below shows a definite barchan.

  • Dark dunes (probably basalt), in an intracrater dune field, Noachis. Picture from Mars Global Surveyor, under the MOC Public Targeting Program.

  • Wide view of dunes in Noachis, as seen by HiRISE.

  • Close-up View of dunes in previous image, as seen by HiRISE. Note how sand barely covers some boulders.

  • Wide view of a field of sand dunes

  • Close view of sand dunes A barchan dune is labeled.

  • Close view of sand dunes, as seen by HiRISE under HiWish program

  • Close view of sand dunes A barchan dune is labeled.

  • Close, color view of sand dunes

  • Close, color view of dome sand dunes, as seen by HiRISE underHiWish program

Gullies

Gullies on steep slopes are found in certain regions of Mars. Many ideas have been advanced to explain them. Formation by running water when the climate was different is a popular idea. Recently, because changes in gullies have been seen since HiRISE has been orbiting Mars, it is thought that they may be formed by chunks of dry ice moving down slope during spring time. Gullies are one of the most interesting discoveries made by orbiting space craft.[16] [17] [18] [19]


  • Wide view of gullies and ridges in crater Ridges may be from old glaciers.

  • Close view of gully channels Arrows point to small channel within larger channels.

  • Wide view of gullies, as seen by HiRISE under HiWish program

  • Close view of gullies Channels show curves.

  • Close view of gullies, as seen by HiRISE under HiWish program Polygonal shapes are visible.

  • Crater with gullies

  • Close view of gullies

Hellas floor features

The Hellas floor contains some strange-looking features. One of these features is called "banded terrain."[20] [21] [22] This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.[23] Banded terrain is found in the north-western part of the Hellas basin. This is the deepest part of the Hellas basin. The banded-terrain deposit displays an alternation of narrow band shapes and inter-bands. The sinuous nature and relatively smooth surface texture suggesting a viscous flow origin. A study published in Planetary and Space Science found that this terrain was the youngest deposit of the interior of Hellas. They also suggest in the paper that banded terrain may have covered a larger area of the NW interior of Hellas. The bands can be classified as linear, concentric, or lobate. Bands are typically 3–15 km long, 3 km wide. Narrow inter-band depressions are 65 m wide and 10 m deep.[24] Pictures of these features can look like abstract art.

  • Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE

  • Twisted Terrain in Hellas Planitia, but actually located in Noachis quadrangle. Imagine trying to walk across this. Image taken with HiRISE.

  • Layered features on floor of Hellas Planitia This may be an example of honeycomb terrain that is not yet completely understood.

  • Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program

  • Twisted bands on the floor of Hellas Planitia These twisted bands are also called "taffy pull" terrain.

  • Wide view of twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program

  • Floor features in Hellas Planitia

Gullies on Dunes

Gullies are found on some dunes. These are somewhat different than gullies in other places, like the walls of craters. Gullies on dunes seem to keep the same width for a long distance and often just end with a pit, instead of an apron. Many of these gullies are found on dunes in Russell Crater.

  • Wide view of dunes in Russell Crater, as seen by HiRISE Many narrow gullies are visible.

  • Close view of the end of gullies in Russell Crater Note: These type of gullies do not usually end with an apron.

  • Close view of the end of gullies in Russell Crater

  • Close, color view of the end of gullies in Russell Crater, as seen by HiRISE

Channels

  • Channels

  • Channel, as seen by HiRISE under HiWish program

Other scenes from Noachis quadrangle

  • Ridges, as seen by HiRISE under HiWish program

  • High center polygons Boxes are drawn around two individual polygons.

  • Wide view of mounds and brain terrain

  • Close view of mounds and brain terrain

  • Light-toned material Light-toned material is often associated with minerals that formed in water.

  • Close view of surface, showing boulders and light-toned material

  • Flow or glacier

  • Wide view showing flows and ridges

See also

External links

References

  1. ↑ http://themis.asu.edu/zoom-20040317a%7Ctitle=Exhumed Crater (Released 17 March 2004)|author=Mars Space Flight Facility|date=17 March 2004|publisher=Arizona State University|
  2. ↑ Lefort | first1 = A. | display-authors = etal | year = 2010 | title = Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE | url = | journal = Icarus | volume = 205 | issue = 1| pages = 259–268 |
  3. ↑ Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY, NY.
  4. ↑ https://www.uahirise.org/PSP_004340_1235 | title=HiRISE | Scalloped Depressions in Peneus Patera (PSP_004340_1235)}}
  5. ↑ McEwen, A., et al. 2017. Mars The Pristine Beauty of the Red Planet. University of Arizona Press. Tucson.
  6. ↑ doi=10.1038/nature02114 |pmid=14685228 |title=Recent ice ages on Mars |journal=Nature |volume=426 |issue=6968 |pages=797–802 |year=2003 |last1=Head |first1=James W. |last2=Mustard |first2=John F. |last3=Kreslavsky |first3=Mikhail A. |last4=Milliken |first4=Ralph E. |last5=Marchant |first5=David R. |
  7. ↑ |doi=10.1016/j.icarus.2015.07.033 |title=Modeling the development of martian sublimation thermokarst landforms |journal=Icarus |volume=262 |pages=154–169 |year=2015 |last1=Dundas |first1=Colin M. |last2=Byrne |first2=Shane |last3=McEwen |first3=Alfred S. |https://zenodo.org/record/1259051/files/article.pdf
  8. ↑ Lefort, A.; et al. (2010). "Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE". Icarus. 205 (1): 259–268.
  9. ↑ https://en.wikipedia.org/wiki/Micrometre
  10. ↑ http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412a.html%7Cpublisher=National Aeronautics and Space Administration
  11. ↑ https://web.archive.org/web/20111028015730/http://mars.jpl.nasa.gov/spotlight/kenEdgett.html |
  12. ↑ doi=10.1016/j.icarus.2011.06.011 |title=Multitemporal observations of identical active dust devils on Mars with the High Resolution Stereo Camera (HRSC) and Mars Orbiter Camera (MOC) |journal=Icarus |volume=215 |issue=1 |pages=358–369 |year=2011 |last1=Reiss |first1=D. |last2=Zanetti |first2=M. |last3=Neukum |first3=G. |
  13. ↑ http://www.lpi.usra.edu/publications/slidesets/stones/ | title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}
  14. ↑ Hugh H. Kieffer|title=Mars|url=https://books.google.com/books?id=NoDvAAAAMAAJ%7Caccessdate=7 March 2011|date=1992|publisher=University of Arizona Press|isbn=978-0-8165-1257-7
  15. ↑ Pye|first=Kenneth|title=Aeolian Sand and Sand Dunes|year=2008|publisher=Springer|isbn=9783540859109|pages=138|
  16. ↑ http://www.jpl.nasa.gov/news/news.php?release=2014-226 | title=NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars
  17. ↑ http://hirise.lpl.arizona.edu/ESP_032078_1420 | title=HiRISE | Activity in Martian Gullies (ESP_032078_1420)
  18. ↑ http://www.space.com/26534-mars-gullies-dry-ice.html | title=Gullies on Mars Carved by Dry Ice, Not Water
  19. ↑ http://spaceref.com/mars/frosty-gullies-on-mars.html | title=Frosty Gullies on Mars - SpaceRef
  20. ↑ Diot, X., et al. 2014. The geomorphology and morphometry of the banded terrain in Hellas basin, Mars. Planetary and Space Science: 101, 118-134.
  21. ↑ http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html | title=NASA - Banded Terrain in Hellas
  22. ↑ http://hirise.lpl.arizona.edu/ESP_016154_1420 | title=HiRISE | Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)
  23. ↑ Bernhardt, H., et al. 2018. THE BANDED TERRAIN ON THE HELLAS BASIN FLOOR, MARS: GRAVITY-DRIVEN FLOW NOT SUPPORTED BY NEW OBSERVATIONS. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 1143.pdf
  24. ↑ Complex geomorphologic assemblage of terrains in association with the banded terrain in Hellas basin, Mars |journal=Planetary and Space Science |volume=121 |pages=36–52 |year=2016 |last1=Diot |first1=X. |last2=El-Maarry |first2=M.R. |last3=Schlunegger |first3=F. |last4=Norton |first4=K.P. |last5=Thomas |first5=N. |last6=Grindrod |first6=P.M. |last7=Chojnacki |first7=M. |bibcode=2016P&SS..121...36D |url=https://boris.unibe.ch/74530/1/Diot_Schlunegger.pdf

References

External links

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