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Columbia Hills (Mars)

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Range of low hills inside Gusev crater on Mars
This article is about the hills on Mars. For the hills in Washington State, United States, seeColumbia Hills (Washington).
The view of Columbia Hills from theSpirit landing site

TheColumbia Hills are a range of low hills insideGusev crater onMars. They were observed by theMars Exploration RoverSpirit when it landed within the crater in 2004. They were promptly given an unofficial name byNASA since they were the most striking nearby feature on the surface. The hills lie approximately 3 kilometres (1.9 mi) away from the rover's original landing position. The range is named to memorialize theSpace ShuttleColumbia disaster. On February 2, 2004, the individual peaks of the Columbia Hills were named after the sevenastronauts who died in the disaster.Spirit spent a few years exploring the Columbia Hills until it ceased to function in 2010. It was also considered a potential landing site for theMars 2020Perseverance rover,[1] before the selection ofJezero crater in November 2018.[2]

Peaks

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The seven peaks are, from north to south:

Rocks and Minerals of Columbia Hills

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Unlabelled overhead view of the Columbia Hills. A labelled version is availablehere.

With theSpirit rover, scientists found a variety of rock types in the Columbia Hills, and they placed them into six different categories, each named after a prominent rock in the respective group: Clovis, Wishbone, Peace, Watchtower, Backstay, and Independence. Their chemical compositions, as measured by APXS, are significantly different from each other.[3] Most importantly, all of the rocks in Columbia Hills show various degrees of alteration by aqueous fluids.[4]They are enriched in the elementsphosphorus,sulfur,chlorine, andbromine—all of which can be carried around in water solutions. The Columbia Hills’ rocks contain basaltic glass, along with varying amounts ofolivine andsulfates.[5][6]The olivine abundance varies inversely with the amount of sulfates. This is exactly what is expected because water destroys olivine but helps to produce sulfates.

Acid fog is believed to have changed some of the Watchtower rocks. This was in a 200 meter long section of Cumberland Ridge and the Husband Hill summit. Certain places became less crystalline and more amorphous. Acidic water vapor from volcanoes dissolved some minerals forming a gel. When water evaporated a cement formed and produced small bumps. This type of process has been observed in the lab when basalt rocks are exposed to sulfuric andhydrochloric acids.[7][8][9]

The Clovis group is especially interesting because theMössbauer spectrometer (MB) detectedgoethite in it.[10] Goethite forms only in the presence ofwater, so its discovery is the first direct evidence of past water in the Columbia Hills's rocks. In addition, the MB spectra of rocks and outcrops displayed a strong decline in olivine presence,[11] although the rocks probably once contained much olivine.[12] Olivine is a marker for the lack of water because it easily decomposes in the presence of water. Sulfate was found, and it needs water to form.

Wishstone contained a great deal ofplagioclase, someolivine, andanhydrite (a calcium sulfate). Peace rocks showedsulfur and strong evidence for bound water, so hydrated sulfates are suspected. Watchtower class rocks lack olivine, implying that they may have been altered by water. The Independence class showed some signs ofclay (perhapsmontmorillonite, a member of thesmectite group). Clays require fairly long term exposure to water to form.

One type of soil, called Paso Robles, from the Columbia Hills, may be an evaporate deposit because it contains large amounts of sulfur,phosphorus,calcium, andiron.[13]Also, MB found that much of the iron in Paso Robles soil was of the oxidized, Fe+++ form, which would happen if water had been present.[14]

Towards the middle of the six-year mission (a mission that was supposed to last only 90 days), large amounts of puresilica were found in the soil. The silica could have come from the interaction of soil with acid vapors produced by volcanic activity in the presence of water or from water in a hot spring environment.[15]

AfterSpirit stopped working scientists studied old data from the Miniature Thermal Emission Spectrometer (Mini-TES) and confirmed the presence of large amounts ofcarbonate-rich rocks, which means that regions of the planet may have once harbored water. The carbonates were discovered in an outcrop of rocks called "Comanche."[16][17]

See also

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References

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  1. ^"Scientists Shortlist Three Landing Sites for Mars 2020".NASA/JPL. Retrieved2017-02-15.
  2. ^Chang, Kenneth (19 November 2018)."NASA Mars 2020 Rover Gets a Landing Site: A Crater That Contained a Lake - The rover will search the Jezero Crater and delta for the chemical building blocks of life and other signs of past microbes".The New York Times. Retrieved3 December 2018.
  3. ^Squyres, S., et al. 2006 Rocks of the Columbia Hills. J. Geophys. Res. Planets. 111,doi:10.1029/2005JE002562
  4. ^Ming, D., et al. 2006 Geochemical and mineralogical indicators for aqueous processes in the Columbia Hills of Gusev crater, Mars. J. Geophys: Res.111,doi:10.1029/2005JE002560
  5. ^Schroder, C., et al. (2005) European Geosciences Union, General Assembly, Geophysical Research abstr., Vol. 7, 10254, 2005
  6. ^Christensen, P.R. (2005) Mineral Composition and Abundance of the Rocks and Soils at Gusev and Meridiani from the Mars Exploration Rover Mini-TES Instruments AGU Joint Assembly, 23–27 May 2005http://www.agu.org/meetings/sm05/waissm05.htmlArchived 2013-05-13 at theWayback Machine
  7. ^"Signs of Acid Fog Found on Mars - SpaceRef". 2 November 2015. Archived fromthe original on August 29, 2016.
  8. ^"Abstract: IN-SITU EVIDENCE FOR ALTERATION BY ACID FOG ON HUSBAND HILL, GUSEV CRATER, MARS (2015 GSA Annual Meeting in Baltimore, Maryland, USA (1-4 November 2015))".
  9. ^COLE, Shoshanna B., et al. 2015. IN-SITU EVIDENCE FOR ALTERATION BY ACID FOG ON HUSBAND HILL, GUSEV CRATER, MARS. 2015 GSA Annual Meeting in Baltimore, Maryland, USA (1-4 November 2015)Paper No. 94-10
  10. ^Klingelhofer, G., et al. (2005) Lunar Planet. Sci. XXXVI abstr. 2349
  11. ^Schroder, C., et al. (2005) European Geosciences Union, General Assembly, Geophysical Research abstr., Vol. 7, 10254, 2005
  12. ^Morris, S., et al. Mossbauer mineralogy of rock, soil, and dust at Gusev crater, Mars:Spirit's journal through weakly altered olivine basalt on the plains and pervasively altered basalt in the Columbia Hills. J. Geophys. Res.: 111
  13. ^Ming, D., et al. 2006 Geochemical and mineralogical indicators for aqueous processes in the Columbia Hills of Gusev crater, Mars. J. Geophys. Res.111
  14. ^Bell, J (ed.) The Martian Surface. 2008. Cambridge University Press.ISBN 978-0-521-86698-9
  15. ^"NASA - Mars Rover Spirit Unearths Surprise Evidence of Wetter Past". Archived fromthe original on 2013-03-08. Retrieved2012-01-16.
  16. ^"Outcrop of long-sought rare rock on Mars found".
  17. ^Richard V. Morris, Steven W. Ruff, Ralf Gellert, Douglas W. Ming, Raymond E. Arvidson, Benton C. Clark, D. C. Golden, Kirsten Siebach, Göstar Klingelhöfer, Christian Schröder, Iris Fleischer, Albert S. Yen, Steven W. Squyres. Identification of Carbonate-Rich Outcrops on Mars by the Spirit Rover.Science, June 3, 2010doi:10.1126/science.1189667

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