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Chasma

From Wikipedia, the free encyclopedia
Deep, elongated, steep-sided depression on a planetary surface
Not to be confused withChasm.

Inplanetary nomenclature, achasma/ˈkæzmə/ (plural:chasmata/ˈkæzmətə/) is a deep, elongated, steep-sideddepression.[1] As of 2020, theIAU has named 122 such features in the Solar System, onVenus (63),Mars (25), Saturn's satellitesMimas (6),Tethys (2),Dione (8) andRhea (5), Uranus's satellitesAriel (7),Titania (2) andOberon (1) and Pluto's satelliteCharon (3). An example isEos Chasma onMars.

Mars

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Below are images of some of the major chasmata of Mars. The map shows their relative locations.

Interior layered deposits and sulfate

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Parts of the floor of Candor Chasma contains layered deposits that have been termed interior layered deposits (ILD's). These layers may have formed when the whole area was a giant lake. Some places on Mars contain hydratedsulfate deposits. Sulfate formation involves the presence of water. TheEuropean Space Agency'sMars Express found evidence of perhapsepsomite andkieserite. Scientists want to visit these areas with robotic rovers.[2]

Layers

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Images of rocks in the canyon walls almost always show layers. Some layers appear tougher than others. In the image below ofGanges Chasma Layers, as seen byHiRISE, one can see that the upper, light-toned deposits are eroding much faster than the lower darker layers. Some cliffs on Mars show a few darker layers standing out and often breaking into large pieces; these are thought to be hard volcanic rock instead of soft ash deposits. An example of hard layers is shown below in the picture of layers in the canyon wall in Coprates, as seen byMars Global Surveyor. Because of its closeness to the Tharsis volcanic region, the rock layers may be made of layer after layer oflava flows, probably mixed with deposits of volcanic ash that fell out of the air following big eruptions. It is likely the rock strata in the walls preserve a long geological history of Mars.[3] Dark layers may be due to dark lava flows. The dark volcanic rockbasalt is common on Mars. However, light-toned deposits may have resulted from rivers, lakes, volcanic ash, or wind blown deposits of sand or dust.[4] TheMars Rovers found light-toned rocks to containsulfates. Probably having been formed in water, sulfate deposits are of great interest to scientists because they may contain traces of ancient life.[5]

Hebes Chasma and hydrated deposits

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Hebes Chasma, a large enclosed valley, may have once held water. Hydrated minerals have been found there. It is thought that large-scale underground springs of groundwater at different times burst to the surface to form deposits called Light Toned Deposits (LTD's). Some suggest present or fossilized life forms may be found there because the deposits are relatively young.[6]

  • Map of Coprates quadrangle showing details of Valles Marineris, the largest canyon system in the solar system. Some of the canyons may have once been filled with water. The map shows the locations of a number of major Chasma.
    Map of Coprates quadrangle showing details ofValles Marineris, the largest canyon system in the solar system. Some of the canyons may have once been filled with water. The map shows the locations of a number of major Chasma.
  • False color image of Candor Chasma showing locations of hydrated sulfate deposits, as seen by THEMIS. Red colors show rocky places. Greens and blues show sandy, dusty areas.
    False color image ofCandor Chasma showing locations of hydratedsulfate deposits, as seen byTHEMIS. Red colors show rocky places. Greens and blues show sandy, dusty areas.
  • Melas Chasma, as seen by THEMIS. Click on image to see relationship of Melas to other features.
    Melas Chasma, as seen byTHEMIS. Click on image to see relationship of Melas to other features.
  • Cliff in Candor Chasma Plateau, as seen by THEMIS. Click on image to see relationship with other features in Coprates quadrangle.
    Cliff inCandor Chasma Plateau, as seen byTHEMIS. Click on image to see relationship with other features in Coprates quadrangle.
  • Cliff in northern wall of Ganges Chasma, as seen by THEMIS. Click on image to see relationship with other features in the Coprates quadrangle.
    Cliff in northern wall ofGanges Chasma, as seen byTHEMIS. Click on image to see relationship with other features in the Coprates quadrangle.
  • Ophir Chasma Wall, as seen by HiRISE.
    Ophir Chasma Wall, as seen byHiRISE.
  • Ius Chasma, as seen by HiRISE. Click on image to see layers.
    Ius Chasma, as seen byHiRISE. Click on image to see layers.
  • Tithonium Chasma Layers, as seen by HiRISE.
    Tithonium Chasma Layers, as seen byHiRISE.
  • Ganges Chasma Layers, as seen by HiRISE.
    Ganges Chasma Layers, as seen byHiRISE.

See also

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  • Geology of Mars – Scientific study of the surface, crust, and interior of the planet Mars

References

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  1. ^"Planetary Names: Descriptor Terms (Feature Types)".planetarynames.wr.usgs.gov.Archived from the original on 2020-08-25. Retrieved5 May 2018.
  2. ^"Bath Salts in Candor Chasma? - Mars Odyssey Mission THEMIS".themis.asu.edu.Archived from the original on 29 September 2009. Retrieved5 May 2018.
  3. ^"Landslides and Debris in Coprates Chasma - Mars Odyssey Mission THEMIS".themis.asu.edu.Archived from the original on 29 September 2009. Retrieved5 May 2018.
  4. ^"HiRISE - Light-toned Layers in Eos Chaos (PSP_005385_1640)".hirise.lpl.arizona.edu.Archived from the original on 3 January 2018. Retrieved5 May 2018.
  5. ^"Stratigraphy Exposed in Ius Chasma". 2008-10-08.
  6. ^http://www.universetoday.com/2008/12/11/Groundwater May Have Played Important Role in Shaping Mars

External links

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