Difference between revisions of "Noachis quadrangle"
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Revision as of 14:47, 8 March 2020
| 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, classical names for regions on Mars. Noachis is considered among the oldest regions on Mars since it is so densely covered with impact craters that ii. 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]
Contents
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]
- PSP 004340 1235scalloped.jpg
Scalloped topography, as seen by HiRISE
- 4340 1235scalloped.jpg
Close view of scalloped topography, as seen by HiRISE
- ESP 050715 1225devilsscallops.jpg
Scalloped topography, as seen by HiRISE under HiWish program Dust devil tracks are also visible.
- ESP 050728 1210scalloped.jpg
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] The pattern of the dust devil tracks have been shown to change every few months.[10] 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.[11] 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.[12] 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.[13] The image below of Russel Crater shows changes in dust devil tracks over a period of only three months, as documented by HiRISE. Other Dust Devil Tracks are visible in the picture of Frento Vallis.
- Russel Crater Dust Devil Changes.JPG
Russell Crater Dust Devil Changes, as seen by HiRISE. Click on image to see changes in dust devil tracks in just 3 months.
- Frento Vallis.JPG
Frento Vallis, as seen by HiRISE. Click on image to see better view of Dust Devil Tracks.
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.[14] The peak is caused by a rebound of the crater floor following the impact.[15] Sometimes craters will display layers. Craters can show us what lies deep under the surface.
- Maunder Crater.JPG
Maunder Crater, as seen by HiRISE. The overhang is part of the degraded south (toward bottom) wall of crater. The scale bar is 500 meters long.
- Asimov Crater.jpg
Asimov Crater, as seen by HiRISE. Bottom of picture shows southeastern wall of crater. Top of picture is edge of mound that fills most of the crater.
- Asimov Crater Layers.jpg
Layers in west slope of Asimov Crater, as seen by HiRISE.
- Asimov Layers Close-up.JPG
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.
- Asimov Crater Central Pit.jpg
East Slope of Central Pit in Asimov Crater, as seen by HiRISE. Click on image to see more details of the many gullies.
- Kaiser Crater.JPG
Kaiser Crater (large crater in upper part of image)context for THEMIS image.
- Kaiser Crater.jpg
Detail of south wall of Kaiser Crater, as seen by THEMIS. Top of image shows part of a dune field.
- Rabe Crater Floor.JPG
Rabe Crater Floor, as seen by HiRISE. Click on image to see layers. Dark sand that made the dunes was probably blown in from elsewhere.
- Exhumed crater in Noachis.JPG
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.
- 24396floor.jpg
Floor of crater in Noachis quadrangle, as seen by HiRISE under HiWish program.
- ESP 035632 1490noachiscraterfloor.jpg
Erosion forms on floor of crater, as seen by HiRISE under HiWish program
- Wikileverrier.jpg
Le Verrier (Martian Crater), as seen by CTX camera (on Mars Reconnaissance Orbiter)
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.[16] One picture below shows a definite barchan.
- Dark dunes in Noachis.JPG
Dark dunes (probably basalt), in an intracrater dune field, Noachis. Picture from Mars Global Surveyor, under the MOC Public Targeting Program.
- Dunes Wide View.jpg
Wide view of dunes in Noachis, as seen by HiRISE.
- Close-up view of Dunes.jpg
Close-up View of dunes in previous image, as seen by HiRISE. Note how sand barely covers some boulders.
- Barchan in Noachis.jpg
Barchan sand dunes in the Hellespontus region, as seen by HiRISE. The horns point in the downwind direction.
- Proctor Crater Ripples and Dunes.JPG
Proctor Crater ripples and dunes, as seen by HiRISE.
- ESP 046378 1415dunes.jpg
Wide view of a field of sand dunes, as seen by HiRISE under HiWish program
- 46378 1415dunes.jpg
Close view of sand dunes, as seen by HiRISE under HiWish program A birchen dune is labeled.
- 46378 1415dunes2.jpg
Close view of sand dunes, as seen by HiRISE under HiWish program
- 46378 1415dunes3.jpg
Close view of sand dunes, as seen by HiRISE under HiWish program A birchen dune is labeled.
Close, color view of sand dunes, as seen by HiRISE under HiWish program
- 55097 1455dunescolor.jpg
Close, color view of dome sand dunes, as seen by HiRISE under HiWish 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.[17] [18] [19] [20]
- ESP 037793 1445noachisgullies.jpg
Gullies on the wall of a crater, as seen by HiRISE under HiWish program
- Close-up of Asimov Crater.JPG
Gullies on mound in Asimov Crater, as seen by HiRISE
- ESP 048159 1310gullies.jpg
Wide view of gullies and ridges in crater, as seen by HiRISE under HiWish program
- 48159 1310gullychannels.jpg
Close view of gully channels, as seen by HiRISE under HiWish program Channels make some tight curves.
- 48159 1310gullychannelsclose.jpg
Close view of gully channels, as seen by HiRISE under HiWish program Arrows point to small channel within larger channels.
- ESP 055056 1420gulliesridges.jpg
Wide view of gullies, as seen by HiRISE under HiWish program
- 55056 1420gullies.jpg
Close view of gullies, as seen by HiRISE under HiWish program Channels show curves.
- 55056 1420gulliesclose.jpg
Close view of gullies, as seen by HiRISE under HiWish program Polygonal shapes are visible.
- ESP 055227 1420crater.jpg
Crater with gullies, as seen by HiRISE under HiWish program
- 55227 1420gullies.jpg
Close view of gullies, as seen by HiRISE under HiWish program
Hellas floor features
The Hellas floor contains some strange-looking features. One of these features is called "banded terrain."[21] [22] [23] This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.[24] 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.[25] Pictures of these features can look like abstract art.
- G18 025437 1406hellasbandssuperwide.jpg
Wide view of part of the floor of the Hellas basin, as seen by CTX
- G18 025437 1406hellasbandswide.jpg
Wide view of Hellas basin floor, as seen by CTX. This is a slight enlargement of the previous image. The box shows the location of the next image that was taken with HiRISE.
- ESP 033995 1410bands.jpg
Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE Other, previous photos show wide views of this region.
- Twisted Terrain in Hellas Planitia.jpg
Twisted Terrain in Hellas Planitia, but actually located in Noachis quadrangle. Imagine trying to walk across this. Image taken with HiRISE.
- ESP 048830 1415ridges.jpg
Layered features on floor of Hellas Planitia, as seen by HiRISE under HiWish program This may be an example of honeycomb terrain that is not yet completely understood.
- ESP 055080 1425twistedbands.jpg
Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program
- ESP 055212 1420taffypull.jpg
Twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program These twisted bands are also called "taffy pull" terrain.
- ESP 055146 1425ridges.jpg
Wide view of twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program
- 55146 1425ridgesclosecolor.jpg
Close view of ridges in twisted bands, as seen by HiRISE under HiWish program
- ESP 055001 1425honeycomb.jpg
Floor features in Hellas Planitia, as seen by HiRISE under HiWish program
- ESP 055067 1420ridgenetwork.jpg
Floor features in Hellas Planitia, as seen by HiRISE under HiWish program
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.
- ESP 020217 1255dunechannels.jpg
Wide view of dunes in Russell Crater, as seen by HiRISE Many narrow gullies are visible.
- 20217 1255dunechannelsclose.jpg
Close view of the end of gullies in Russell Crater, as seen by HiRISE Note: These type of gullies do not usually end with an apron.
- 20217 1255dunechannelsclosetop.jpg
Close view of the end of gullies in Russell Crater, as seen by HiRISE
Close, color view of the end of gullies in Russell Crater, as seen by HiRISE
Channels
- ESP 056981 1415channels.jpg
Channels, as seen by HiRISE under HiWish program
- ESP 053698 1485channel.jpg
Channel, as seen by HiRISE under HiWish program
Other scenes from Noachis quadrangle
- Dissected Mantle.JPG
Dissected Mantle with layers, as seen by HiRISE.
- Esp 037147 1430layers.jpg
Layers in depression in crater, as seen by HiRISE under HiWish program
- ESP 046417 1425twistedridges.jpg
Wide view of ridges, as seen by HiRISE under HiWish program
- 46417 1425hollows.jpg
Close view of hollows, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image.
- 46417 1425straightridges.jpg
Ridges, as seen by HiRISE under HiWish program Note: this is an enlargement of the previous image.
- 48159 1310highcenterpolygons.jpg
High center polygons, as seen by HiRISE under HiWish program Boxes are drawn around two individual polygons.
- ESP 048184 1470moundsbrains.jpg
Wide view of mounds and brain terrain, as seen by HiRISE under HiWish program
- 48184 1470moundsbrains.jpg
Close view of mounds and brain terrain, as seen by HiRISE under HiWish program
- ESP 049226 1480boulderslighttoned.jpg
Light-toned material, as seen by HiRISE under HiWish program Light-toned material is often associated with minerals that formed in water.
- 49226 1480boulderslighttoned.jpg
Close view of surface, showing boulders and light-toned material, as seen by HiRISE under HiWish program
- ESP 049674 1470flow.jpg
Flow, as seen by HiRISE under HiWish program
- ESP 051138 1460ridges.jpg
Wide view showing flows and ridges, as seen by HiRISE under HiWish program
- 51138 1460ridges.jpg
Close view of ridges, as seen by HiRISE under HiWish program
See also
- Dark slope streaks
- Geography of Mars
- High Resolution Imaging Science Experiment (HiRISE)
- HiWish program
- How are features on Mars Named?
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
- https://www.youtube.com/watch?v=PYl3HXpvqhM Kris Zacny Water on Mars - 21st Annual International Mars Society Convention Describes how to get water from ice in the ground]
References
- ↑ 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|
- ↑ 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 |
- ↑ Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY, NY.
- ↑ https://www.uahirise.org/PSP_004340_1235 | title=HiRISE | Scalloped Depressions in Peneus Patera (PSP_004340_1235)}}
- ↑ McEwen, A., et al. 2017. Mars The Pristine Beauty of the Red Planet. University of Arizona Press. Tucson.
- ↑ 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. |
- ↑ |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
- ↑ 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.
- ↑ https://en.wikipedia.org/wiki/Micrometre
- ↑ http://mars.jpl.nasa.gov/spotlight/KenEdgett.html |title=Ken Edgett |date=2001 |publisher=National Aeronautics and Space Administration
- ↑ http://marsrovers.jpl.nasa.gov/gallery/press/spirit/20070412a.html%7Cpublisher=National Aeronautics and Space Administration
- ↑ https://web.archive.org/web/20111028015730/http://mars.jpl.nasa.gov/spotlight/kenEdgett.html |
- ↑ 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. |
- ↑ http://www.lpi.usra.edu/publications/slidesets/stones/ | title=Stones, Wind, and Ice: A Guide to Martian Impact Craters}}
- ↑ 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
- ↑ Pye|first=Kenneth|title=Aeolian Sand and Sand Dunes|year=2008|publisher=Springer|isbn=9783540859109|pages=138|
- ↑ http://www.jpl.nasa.gov/news/news.php?release=2014-226 | title=NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars
- ↑ http://hirise.lpl.arizona.edu/ESP_032078_1420 | title=HiRISE | Activity in Martian Gullies (ESP_032078_1420)
- ↑ http://www.space.com/26534-mars-gullies-dry-ice.html | title=Gullies on Mars Carved by Dry Ice, Not Water
- ↑ http://spaceref.com/mars/frosty-gullies-on-mars.html | title=Frosty Gullies on Mars - SpaceRef
- ↑ Diot, X., et al. 2014. The geomorphology and morphometry of the banded terrain in Hellas basin, Mars. Planetary and Space Science: 101, 118-134.
- ↑ http://www.nasa.gov/mission_pages/MRO/multimedia/20070717-2.html | title=NASA - Banded Terrain in Hellas
- ↑ http://hirise.lpl.arizona.edu/ESP_016154_1420 | title=HiRISE | Complex Banded Terrain in Hellas Planitia (ESP_016154_1420)
- ↑ 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
- ↑ 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
- [https://www.youtube.com/watch?v=483HcpqyMNU Banded Flow Terrain in Hellas Basi
