Difference between revisions of "Layers on Mars"
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Layers show up in the walls of craters. | Layers show up in the walls of craters. | ||
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File: 57080 1380layerscratercolor.jpg|Layers in crater wall in Phaethontis quadrangle, as seen by HiRISE under HiWish program | File: 57080 1380layerscratercolor.jpg|Layers in crater wall in Phaethontis quadrangle, as seen by HiRISE under HiWish program | ||
File:ESP 057098 2050layers.jpg|Layers around crater in Syrtis Major quadrangle | File:ESP 057098 2050layers.jpg|Layers around crater in Syrtis Major quadrangle | ||
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==Canyons and troughs== | ==Canyons and troughs== | ||
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File:Troughs in Elysium Planitia.jpg|Troughs displaying layers in the Elysium Planitia | File:Troughs in Elysium Planitia.jpg|Troughs displaying layers in the Elysium Planitia | ||
File:43376 1710layersclose.jpg|Layers in a trough in Coprates quadrangle | File:43376 1710layersclose.jpg|Layers in a trough in Coprates quadrangle | ||
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==Along ancient river valleys== | ==Along ancient river valleys== | ||
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<gallery class="center" widths="190px" heights="180px" > | <gallery class="center" widths="190px" heights="180px" > | ||
File:Shalbatana Vallis.JPG|Layers in wall of Shalbatana Vallis | File:Shalbatana Vallis.JPG|Layers in wall of Shalbatana Vallis | ||
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==Islands of layers== | ==Islands of layers== | ||
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File:47080 2120layersclose.jpg|Layers in mesa in Mare Acidalium quadrangle | File:47080 2120layersclose.jpg|Layers in mesa in Mare Acidalium quadrangle | ||
File:47441 1800mesaclose.jpg|Mesa with box showing size of football field | File:47441 1800mesaclose.jpg|Mesa with box showing size of football field | ||
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Pedestal craters develop a protective top layer from the action of crater ejecta. | Pedestal craters develop a protective top layer from the action of crater ejecta. | ||
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File:ESP 047367 1910pedestal.jpg|Wide view of pedestal The southern (lower) edge is enlarged in next image to show layers. | File:ESP 047367 1910pedestal.jpg|Wide view of pedestal The southern (lower) edge is enlarged in next image to show layers. | ||
File:47367 1910pedestallayerssouth.jpg|Close view of layers in pedestal crater in Arabia quadrangle | File:47367 1910pedestallayerssouth.jpg|Close view of layers in pedestal crater in Arabia quadrangle | ||
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==Inside craters== | ==Inside craters== | ||
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File:56818 1790layersshadows.jpg|Layers in depression on crater floor | File:56818 1790layersshadows.jpg|Layers in depression on crater floor | ||
File:ESP 042055 1580layers.jpg| Layers in depression on crater floor | File:ESP 042055 1580layers.jpg| Layers in depression on crater floor | ||
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Large masses of layered deposits in depressions, such as craters have been called '''Equatorial Layered Deposits''' (ELD’s) or Interior Layered Deposits (ILDs) in Valles Marineris.<ref >Lucchitta B., et al. 1992 In Mars, 453-492. University of Arizona Press. Tucson</ref> | Large masses of layered deposits in depressions, such as craters have been called '''Equatorial Layered Deposits''' (ELD’s) or Interior Layered Deposits (ILDs) in Valles Marineris.<ref >Lucchitta B., et al. 1992 In Mars, 453-492. University of Arizona Press. Tucson</ref> | ||
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File:Henry Crater Mound.JPG|Layers exposed on mound in Henry Crater | File:Henry Crater Mound.JPG|Layers exposed on mound in Henry Crater | ||
File:Wikiesp 035896 1845crommelinhollows.jpg|Layered mound on floor of Crommelin Crater | File:Wikiesp 035896 1845crommelinhollows.jpg|Layered mound on floor of Crommelin Crater | ||
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==Mantle layers== | ==Mantle layers== | ||
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File:ESP 050793 1365pyramids.jpg| Wide view of layered features in Hellas quadrangle | File:ESP 050793 1365pyramids.jpg| Wide view of layered features in Hellas quadrangle | ||
File:50793 1365layers2.jpg|Close view of layered features in Hellas quadrangle Each layer may represent a change in the climate. | File:50793 1365layers2.jpg|Close view of layered features in Hellas quadrangle Each layer may represent a change in the climate. | ||
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==Northern polar layers== | ==Northern polar layers== | ||
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File:ESP 044934 2670icecaplayers.jpg|Layers exposed in ice cap in Mare Boreum quadrangle | File:ESP 044934 2670icecaplayers.jpg|Layers exposed in ice cap in Mare Boreum quadrangle | ||
File:ESP 036863 2670icecaplayers.jpg| Layers exposed in ice cap in Mare Boreum quadrangle | File:ESP 036863 2670icecaplayers.jpg| Layers exposed in ice cap in Mare Boreum quadrangle | ||
| − | <gallery> | + | </gallery> |
==Layers created by groundwater== | ==Layers created by groundwater== | ||
Revision as of 07:58, 15 November 2018
Article written by Jim Secosky. Jim is a retired science teacher who has used the Hubble Space Telescope, the Mars Global Surveyor, and HiRISE.
When the pictures from Mariner 9 were examined, scientists thought that with all the craters, Mars must be like the moon. Billions of years of bombardment would have caused the crust to be just broken up rocks they thought. However, this view did not hold up. Mars Global Surveyor from the beginning showed vast areas of layered rocks; layered showed up to 10 km deep in the Valles Marineris. Today, we believe layered is planet-wide. cite journal | doi = 10.1555/mars.2005.0002 | title = The sedimentary rocks of Sinus Meridiani: Five key observations from data acquired by the Mars Global Surveyor and Mars Odyssey orbiters | date = 2005 | last1 = Edgett | first1 = Kenneth S. | journal = The Mars Journal | volume = 1 | pages = 5|</ref> Cite error: Closing </ref> missing for <ref> tag [1] [2] Later, it was determined that indeed Gale Crater once held a lake. [3] [4] [5] [6] The lake in Gale, became full of sediments. Later, all but the center mound was eroded.
This evenly layered rock photographed by the Mast Camera (Mastcam) on NASA's Curiosity Mars Rover shows a pattern typical of a lake-floor sedimentary deposit not far from where flowing water entered a lake.
View from Mastcam on Curiosity showing sloping buttes and layered outcrops on lower Mount Sharp
Many other past lakes have been proposed for craters and other low regions.[7] [8] ref> Cabrol, N., E. Grin. 2001. The evolution of lacustrine environments on Mars: Is Mars only hydrologically dormant. Icarus: 149, 291-328. Cite error: Closing </ref> missing for <ref> tag [9] [10]
Layers on crater floor in Arabia quadrangle
Layers on crater floor, as seen by HiRISE under HiWish program Box shows size of a football field.
Layers in depression on crater floor
Layers in depression on crater floor
Large masses of layered deposits in depressions, such as craters have been called Equatorial Layered Deposits (ELD’s) or Interior Layered Deposits (ILDs) in Valles Marineris.[11] They are often found with outcrops of hydrated sulfates on Mars. Hydrated sulfates are a sign of liquid water in Martian history since they need water to form. Based on albedo, erosion patterns, physical characteristics, and composition, researchers have classified different groups of layers in Gale Crater that seem to be similar to layers in other (ELD’s). The groups include: a small yardang unit, a coarse yardang unit, and a terraced unit.[12] Usually , ELD’s are found ~ ±30° of the equator.[13] Equatorial Layered Deposits appear in various geological settings such as cratered terrains (Arabia Terra, Meridiani Planum), chaotic terrains (Aram Chaos, Aureum Chaos), the Valles Marineris chasmata (and surrounding plateaus), and large impact craters ( Gale, Becquerel, Crommelin). [14] [15] Layering is visible on meter scale, and when the deposits are partly eroded, intricate patterns become visible.[16]
Layers exposed on mound in Henry Crater
Layered mound on floor of Crommelin Crater
Contents
Mantle layers
Another class of layers may have been created as ice-rich material fell from the sky when the climate changed. Because Mars has no large moon to stabilize its tilt, its tilt, and thus its climate vary greatly. At times moisture from the poles enters the atmosphere, and freezes to form snow or ice-coatcoated dust. This ice-rich material collects at mid latitudes. It appears as a smooth covering, called latitude dependent mantle. After each climate change, some of the material stays behind, while much just returns to the Polar Regions. This repeated process results in layers in craters and in sheltered spots like against cliffs. Some of these formations have been shaped by the wind into various shapes. It must be pointed out that mantle is widespread on Mars and contains water ice. This ice can be a major source of water for future colonists.
Wide view of layered features in Hellas quadrangle
Close view of layered features in Hellas quadrangle Each layer may represent a change in the climate.
Northern polar layers
We have known about layers in the northern ice cap for a long time. They are records of many past climate changes.
Layers exposed in ice cap in Mare Boreum quadrangle
Layers exposed in ice cap in Mare Boreum quadrangle
Layers created by groundwater
Although many sets of layers probably originated underwater, some researchers believe that many layered formations were created by a combination of sediment and ground water. [17] [18] [19] [20] [21] Sediment could be transported by the wind, volcanoes, or crater impacts. Water moving through the ground would easily pick up minerals like silica or sulfates that could cement the material. [22] [23] On Earth the hardness of many sedimentary rocks, like sandstone, is mostly from the mineral cement that was put in place as water passed through. Some layers contain Gypsum, a sulfate which forms in relatively fresh water. [24]
Strong proof of groundwater cementing materials comes from the Opportunity Rover. Places, examined by Opportunity such as Endurance, Eagle, and Erebus craters happened to be where the water table breached the surface.[25] [26] [27] In addition, it was found that sediment was transported by wind-driven currents of water in some locations. Groundwater rose and fell, as evidenced by small surface cracks formed during multiple wetting and drying events. Ferric sulfates (such as jarosite) in the rocks of Meridiani Planum indicate that acidic fluids were present. These acidic liquids could have been produced when water with dissolved Fe(II) was oxidized as it reached the surface.[28] Hydrologic models predict that groundwater should indeed emerge in the Sinus Meridiani region which was explored by Opportunity.[29]
What’s so great about layers on Mars
The widespread occurrence of layering on the Red Planet has great significance. On Earth, much layering originates in bodies of water.[30] If this is also true, at least to some extent on Mars, then traces of past life might be found in layered formations. Indeed, much evidence has been gathered for the existence of lakes in craters and some canyons. Whether layers were created under water or through ground water, water is still involved. Most of the organic mass on the Earth is found under the surface.[31] [32] Many microbes live deep underground.[33] [34] [35] Life under the Martian surface might find it easier since it would be protected from high levels of radiation.[36] One recent study found that radiation from certain elements in the crust of Mars could have reacted with water in the ground to produce hydrogen. Hydrogen can supply chemical energy for life.[37] [38]
See also
References
- ↑ https://www.youtube.com/watch?v=fYo31XjoXOk
- ↑ http://apnews.excite.com/article/20120927/DA1IDOO00.html
- ↑ https://www.nasa.gov/press/2014/december/nasa-s-curiosity-rover-finds-clues-to-how-water-helped-shape-martian-landscape
- ↑ https://www.sciencedaily.com/releases/2014/12/141208122903.htm
- ↑ https://www.jpl.nasa.gov/video/details.php?id=1346
- ↑ https://www.jpl.nasa.gov/news/news.php?feature=4398
- ↑ De Hon, R. 1992. Martian lake basins and lacustrine plains. Earth Moon Planets: 56, 95-122.
- ↑ Cabrol, N., E. Grin. 1999. Distribution, classification, and ages of martian impact crater lakes. Icarus: 142, 160-172.
- ↑ Fassett, C. J. Head. 2008. Valley network-fed, open-basin lakes on Mars: Distribution and implications for Noachian surface and subsurface hydrology. Icarus: 198, 37-56.
- ↑ Zhao, J., et al. 2018. PALEOLAKES IN THE NORTHWEST HELLAS REGION: IMPLICATIONS FOR PALEO-CLIMATE AND REGIONAL GEOLOGIC HISTORY. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 1397.pdf
- ↑ Lucchitta B., et al. 1992 In Mars, 453-492. University of Arizona Press. Tucson
- ↑ Le Deit, L., et al. 2011. Geological Comparison of the Gale Crater mount to other equatorial layered deposits (ELDs) on Mars. 42nd Lunar and Planetary Science Conference (2011) 1857.pdf.
- ↑ Malin, M., Edgett, K. 2000. Science: 290,1927.
- ↑ Lucchitta B., et al. 1992 In Mars, 453-492. University of Arizona Press. Tucson
- ↑ Le Deit, L., et al. 2011. Geological Comparison of the Gale Crater mount to other equatorial layered deposits (ELDs) on Mars. 42nd Lunar and Planetary Science Conference (2011) 1857.pdf.
- ↑ http://www.issibern.ch/teams/marsild
- ↑ Grotzinger, J., et al. 2005. Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars. Earth and Planetary Science Letters 240:11–72.
- ↑ Andrews-Hanna J., et al. 2010. Early Mars hydrology: Meridiani playa deposits and the sedimentary record of Arabia Terra. Journal of Geophysical Research 115:E06002.
- ↑ Grotzinger, J., R. Milliken. THE SEDIMENTARY ROCK RECORD OF MARS: DISTRIBUTION, ORIGINS, AND GLOBAL STRATIGRAPHY. 2012. Sedimentary Geology of MarsSEPM Special Publication No. 102, SEPM (Society for Sedimentary Geology), Print ISBN 978-1-56576-312-8, CD/DVD ISBN 978-1-56576-313-5, p. 1–48.
- ↑ Squyres, S. W.; Knoll, A. H. (2005). "Sedimentary rocks at Meridiani Planum: Origin, diagenesis, and implications for life on Mars". Earth Planet. Sci. Lett. 240: 1–10. Bibcode:2005E&PSL.240....1S. doi:10.1016/j.epsl.2005.09.038.
- ↑ Squyres, S. W.; et al. (2006). "Two years at Meridiani Planum: Results from the Opportunity rover". Science. 313: 1403–1407. doi:10.1126/science.
- ↑ https://www.nature.com/articles/ngeo1706
- ↑ Michalski, J., et al. 2013. Groundwater activity on Mars and implications for a deep biosphere. Nature Geoscience volume 6, pages 133–138.
- ↑ cite web|url=http://news.nationalgeographic.com/news/2009/11/091125-mars-crater-lake-michigan-water_2.html |title=Martian "Lake Michigan" Filled Crater, Minerals Hint |publisher=News.nationalgeographic.com |date=2010
- ↑ Grotzinger, J., et al. 2005. Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars. Earth and Planetary Science Letters 240:11–72.
- ↑ Grotzinger J., et al. 2006. Sedimentary textures formed by aqueous processes, Erebus crater, Meridiani Planum, Mars. Geology 34:1085–1088.
- ↑ McLennan S., Grotzinger J. 2008. The sedimentary rock cycle of Mars. In Bell J., (Editor). The Martian Surface: Cambridge University Press, UK. 541–577.
- ↑ Hurowitz J. et al., 2010. Origin of acidic surface waters and the evolution of atmospheric chemistry on early Mars. Nature Geoscience 3:323–326.
- ↑ Andrews-Hanna J., et al. 2007. Meridiani Planum and the global hydrology of Mars. Nature 446:163–166.
- ↑ Namowitz, S., Stone, D. 1975. Earth science The World We Live in. American Book Company. N.Y.
- ↑ https://microbewiki.kenyon.edu/index.php/Deep_subsurface_microbes
- ↑ Amend, J.. A. Teske. 2005. Expanding frontiers in deep subsurface microbiology. Palaeogeography, Palaeoclimatology, Palaeoecology: Volume 219, Issues 1–2, 131-155.
- ↑ Pedersen, K. 1993. The deep subterranean biosphere. Earth Science Reviews: 34, 243-260.
- ↑ Stevens, T., J. McKiney. 1995. Lithoautotrophic Microbial Ecosystems in Deep Basalt Acquifers. Science: 270, 450-454.
- ↑ Fredrickson, J. , T. Onstott. 1996. Microbes Deep inside the Earth. Scientific American. October, 1996.
- ↑ Boston, P., et al. 1992. On the Possibility of Chemosynthetic Ecosystems in Subsurface Habitats on Mars. Icarus: 95, 300-308.
- ↑ http://astrobiology.com/2018/09/ancient-mars-had-right-conditions-for-underground-life.html
- ↑ Tarnas, J., et al. 2018 Radiolytic H2 Production on Noachian Mars: Implications for Habitability and Atmospheric Warming. Earth and Planetary Science Letters [https://doi.org/10.1016/j.epsl.2018.09.001
Recommended reading
- Grotzinger, J. and R. Milliken (eds.). 2012. Sedimentary Geology of Mars. SEPM.
