Difference between revisions of "Noachis quadrangle"
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Image:24396floor.jpg|Floor of crater in Noachis quadrangle, as seen by HiRISE under [[HiWish program]]. | Image:24396floor.jpg|Floor of crater in Noachis quadrangle, as seen by HiRISE under [[HiWish program]]. | ||
| + | File:Secondary craters ESP 081458 1425.jpg|Secondry craters, as seen by HiRISE under HiWish program These were made from material thrown in the air by primary impact of large body nearby. | ||
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Latest revision as of 07:57, 20 February 2024
| MC-27 | Noachis | 30–65° S | 0–60° E | Quadrangles | Atlas |
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. The name "Noachis" means the land of Noah. 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]
In this article, some of the best pictures from a number of spacecraft will show what the landscape looks like in this region. The origins and significance of all features will be explained as they are currently understood.
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] 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
Dust devil tracks and scalloped topography, as seen by HiRISE under HiWish program
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. The pictures show that major changes in dust devil tracks happened in just 3 months.
Craters
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.
Secondry craters, as seen by HiRISE under HiWish program These were made from material thrown in the air by primary impact of large body nearby.
Sand Dunes
Wide view of a field of sand dunes, as seen by Mars Global Surveyor
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.[13] One picture below shows a definite barchan.
Wide view of a field of sand dunes
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.
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.[14] [15] [16] [17]
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
Close-up of banded terrain on the floor of the Hellas basin, as seen by HiRISE
The Hellas floor contains some strange-looking features. One of these features is called "banded terrain."[18] [19] [20] This terrain has also been called "taffy pull" terrain, and it lies near honeycomb terrain, another strange surface.[21] 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.[22] Researchers do not at this time understand how these features ere formed. .[23] [24]
One idea for how these strange features were created involves a large mass of ice being deposited into the Hellas basin. Later the ice could be covered with lava and ash from the many nearby volcanoes. Hot lava would melt some of the ice, but the heat may not have been enough to melt all the ice. So, there may have been a thick layer of lava and ash sitting on top of ice. The ice is much less dense; consequently, it would rise through the denser material that covers it. Strange shapes could result. This principle is like when one pulls a ball down into a swimming pool. The ball would want to go up through the water. On Earth this type of event occurs. The bodies that form are called diapirs. Sometimes salt deposits covered by sediment move upward on the Earth. Diapir comes from Greek diapeirein, which means “to pierce" in reference to how one lower density body pierces or moves through another.[25]
Pictures of these features can look like abstract art.
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.
Floor features in Hellas Planitia
Wide view of twisted bands on the floor of Hellas Planitia, as seen by HiRISE under HiWish program
Banded terrain, 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.
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
- High Resolution Imaging Science Experiment (HiRISE)
- HiWish program
- How are features on Mars Named?
- Mars Global Surveyor
- Martian gullies
- Rivers on Mars
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]
- - Jeffrey Plaut - Subsurface Ice - 21st Annual International Mars Society Convention-2018
- https://www.youtube.com/watch?v=483HcpqyMNU Banded Flow Terrain in Hellas Basin
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://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. |
- ↑ 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
- ↑ https://www.hou.usra.edu/meetings/lpsc2022/pdf/1588.pdf
- ↑ Cook, C., et al. 2022. FORMATION OF THE BANDED TERRAIN OF HELLAS PLANITIA, MARS. 53rd Lunar and Planetary Science Conference (2022). 1588.pdf
- ↑ Fastook1, J. and J. Head. 2023. HELLAS BASIN, MARS: RIM-WALL-FLOOR GLACIATION IN THE LATE NOACHIAN-EARLY HESPERIAN AND INTERACTIONS WITH SUPERPOSED LAVA FLOWS. 54th Lunar and Planetary Science Conference 2023 (LPI Contrib. No. 2806). 1330.pdf
