Martian soil


Martian soil

Martian soil is the fine regolith found on the surface of Mars. Its properties can differ significantly from those of terrestrial soil.

The term Martian soil typically refers to the finer fraction of regolith, that which is composed of grains one centimeter in diameter or less. Some have argued that the term "soil" is not correct in reference to Mars because soil is defined as having organic content, whereas Mars is not known to have any. However, standard usage among planetary scientists is to ignore that distinction. Martian dust generally connotes even finer materials than Martian soil, the fraction which is less than 30 micrometres in diameter. Disagreement over the significance of soil's definition arises due to the lack of an integrated concept of soil in the literature. The pragmatic definition "medium for plant growth" has been commonly adopted in the planetary science community but a more complex definition describes soil as (bio)geochemically/physically altered material at the surface of a planetary body that encompasses surficial extraterrestrial telluric deposits. This definition emphasizes that soil is a body that retains information about its environmental history and that does not need the presence of life to form.

Martian sand and boulders photographed by NASA's Mars Exploration Rover Spirit.

Mars is covered with vast expanses of sand and dust and its surface is littered with rocks and boulders. The dust is occasionally picked up in vast planet-wide dust storms. Mars dust is very fine and enough remains suspended in the atmosphere to give the sky a reddish hue. The reddish hue is due to rusting iron minerals presumably formed a few billion years ago when Mars was warm and wet, but now that Mars is cold and dry, modern rusting may be due to a superoxide that forms on minerals exposed to ultraviolet rays in sunlight.[1] The sand is believed to move only slowly in the Martian winds due to the very low density of the atmosphere in the present epoch. In the past, liquid water flowing in gullies and river vallies may have shaped the Martian regolith. Mars researchers are studying whether groundwater sapping is shaping the Martian regolith in the present epoch, and whether carbon dioxide hydrates exist on Mars and play a role. It is believed that large quantities of water and carbon dioxide ices remain frozen within the regolith in the equatorial parts of Mars and on its surface at higher latitudes. Water contents of Martian regolith range from <2% by weight to more than 60%.[2][3] The presence of olivine, which is an easily weatherable primary mineral, has been interpreted to mean that physical rather than chemical weathering processes currently dominate on Mars.[4]

Regolith beneath NASA's Phoenix Mars Lander, where the descent thrusters have apparently cleared away several patches of soil to expose the underlying ice.

In June, 2008, the Phoenix Lander returned data showing Martian soil to be slightly alkaline and containing vital nutrients such as magnesium, sodium, potassium and chloride, all of which are necessary for living organisms to grow. Scientists compared the soil near Mars' north pole to that of backyard gardens on Earth, and concluded that it could be suitable for growth of plants.[5] However, in August, 2008, the Phoenix Lander conducted simple chemistry experiments, mixing water from Earth with Martian soil in an attempt to test its pH, and discovered traces of the salt perchlorate, while also confirming many scientists theories that the Martian surface was considerably basic, measuring at 8.3. The presence of the perchlorate, if confirmed, would make Martian soil more exotic than previously believed.[6] Further testing is necessary to eliminate the possibility of the perchlorate readings being caused by terrestrial sources, which may have migrated from the spacecraft either into samples or the instrumentation.[7]

While our understanding of Martian soils is extremely rudimentary, their diversity may raise the question of how we might compare them with our Earth-based soils. Applying an Earth-based system is largely debatable but a simple option is to distinguish the (largely) biotic Earth from the abiotic Solar System, and include all non-Earth soils in a new World Reference Base for Soil Resources Reference Group or USDA soil taxonomy Order, which might be tentatively called Astrosols.[8]

Atmospheric dust

Similarly sized dust will settle from the thinner Martian atmosphere sooner than it would on Earth. For example, the dust suspended by the 2001 global dust storms on Mars only remained in the Martian atmosphere for 0.6 years, while the dust from Mt. Pinatubo took about 2 years to settle.[9] However, under current Martian conditions, the mass movements involved are generally much smaller than on Earth. Even the 2001 global dust storms on Mars moved only the equivalent of a very thin dust layer – about 3 µm thick if deposited with uniform thickness between 58° north and south of the equator.[9] Dust deposition at the two rover sites has proceeded at a rate of about the thickness of a grain every 100 sols.[10]

The difference in the concentration of dust in Earth's atmosphere and that of Mars stems from a key factor. On Earth, dust that leaves atmospheric suspension usually gets aggregated into larger particles through the action of soil moisture or gets suspended in oceanic waters. It helps that most of earth's surface is covered by liquid water. Neither process occurs on Mars, leaving deposited dust available for suspension back into the Martian atmosphere.[11] In fact, the composition of Martian atmospheric dust – very similar to surface dust – as observed by the Mars Global Surveyor Thermal Emission Spectrometer, may be volumetrically dominated by composites of plagioclase feldspar and zeolite[12] which can be mechanically derived from Martian basaltic rocks without chemical alteration. Observations of the Mars Exploration Rovers’ magnetic dust traps suggest that about 45% of the elemental iron in atmospheric dust is maximally (3+) oxidized and that nearly half exists in titanomagnetite,[13] both consistent with mechanical derivation of dust with aqueous alteration limited to just thin films of water.[14] Collectively, these observations support the absence of water-driven dust aggregation processes on Mars. Furthermore, wind activity dominates the surface of Mars at present, and the abundant dune fields of Mars can easily yield particles into atmospheric suspension through effects such as larger grains disaggregating fine particles through collisions.[15]

The Martian atmospheric dust particles are generally 3 µm in diameter.[16] It is important to note that while the atmosphere of Mars is thinner, Mars also has a lower gravitational acceleration, so the size of particles that will remain in suspension cannot be estimated with atmospheric thickness alone. Electrostatic and van der Waals forces acting among fine particles introduce additional complexities to calculations. Rigorous modeling of all relevant variables suggests that 3 µm diameter particles can remain in suspension indefinitely at most wind speeds, while particles as large as 20 µm diameter can enter suspension from rest at surface wind turbulence as low as 2 ms−1 or remain in suspension at 0.8 ms−1.[10]

References

  1. ^ Yen, A.S., Kim, S.S., Hecht, M.H., Frant, M.S., Murray, B. (2000). "Evidence that the reactivity of the Martian soil is due to superoxide ions". Science 289 (5486): 1909–12. Bibcode 2000Sci...289.1909Y. doi:10.1126/science.289.5486.1909. PMID 10988066. 
  2. ^ Mitrofanov, I. et 11 al. (2004). "Mineralogy at Gusev crater from the Mössbauer spectrometer on the Spirit rover". Science 297 (5578): 78–81. Bibcode 2002Sci...297...78M. doi:10.1126/science.1073616. PMID 12040089. 
  3. ^ Horneck, G. (2008). "The microbial case for Mars and its implications for human expeditions to Mars". Acta Astronautica 63 (7–10): 1015. doi:10.1016/j.actaastro.2007.12.002. 
  4. ^ Morris, R.V. et 16 al. (2004). "Mineralogy at Gusev crater from the Mössbauer spectrometer on the Spirit rover". Science 305 (5685): 833–6. Bibcode 2004Sci...305..833M. doi:10.1126/science.1100020. PMID 15297666. 
  5. ^ "Martian soil 'could support life'". BBC News. June 27, 2008. http://news.bbc.co.uk/2/hi/science/nature/7477310.stm. Retrieved 2008-08-07. 
  6. ^ Chang, Alicia (2008-08-05). "Scientists: Salt in Mars soil not bad for life". USA Today. Associated Press. http://www.usatoday.com/tech/science/space/2008-08-04-mars-soil_N.htm. Retrieved 2008-08-07. 
  7. ^ "NASA Spacecraft Analyzing Martian Soil Data". JPL. http://www.jpl.nasa.gov/news/phoenix/release.php?ArticleID=1816. Retrieved 2008-08-05. 
  8. ^ Certini, G, Scalenghe, R, Amundson, R (2009). "A view of extraterrestrial soils". European Journal Soil Science 60 (6): 1078. doi:10.1111/j.1365-2389.2009.01173.x. 
  9. ^ a b Cantor, B (2007). "MOC observations of the 2001 Mars planet-encircling dust storm". Icarus 186: 60. Bibcode 2007Icar..186...60C. doi:10.1016/j.icarus.2006.08.019. 
  10. ^ a b Claudin, P; Andreotti, B (2006). "A scaling law for aeolian dunes on Mars, Venus, Earth, and for subaqueous ripples". Earth and Planetary Science Letters 252: 30. arXiv:cond-mat/0603656. Bibcode 2006E&PSL.252...30C. doi:10.1016/j.epsl.2006.09.004. 
  11. ^ Sullivan, R.; Arvidson, R.; Bell, J. F.; Gellert, R.; Golombek, M.; Greeley, R.; Herkenhoff, K.; Johnson, J. et al. (2008). "Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at "El Dorado" and surroundings at Gusev Crater". Journal of Geophysical Research 113: E06S07. Bibcode 2008JGRE..11306S07S. doi:10.1029/2008JE003101. 
  12. ^ Hamilton, Victoria E.; McSween, Harry Y.; Hapke, Bruce (2005). "Mineralogy of Martian atmospheric dust inferred from thermal infrared spectra of aerosols". Journal of Geophysical Research 110: E12006. Bibcode 2005JGRE..11012006H. doi:10.1029/2005JE002501. 
  13. ^ Goetz et al. (2007), Seventh Mars Conference
  14. ^ Goetz, W; Bertelsen, P; Binau, Cs; Gunnlaugsson, Hp; Hviid, Sf; Kinch, Km; Madsen, De; Madsen, Mb; Olsen, M; Gellert, R; Klingelhöfer, G; Ming, Dw; Morris, Rv; Rieder, R; Rodionov, Ds; De, Souza, Pa, Jr; Schröder, C; Squyres, Sw; Wdowiak, T; Yen, A (Jul 2005). "Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust". Nature 436 (7047): 62–5. Bibcode 2005Natur.436...62G. doi:10.1038/nature03807. ISSN 0028-0836. PMID 16001062. 
  15. ^ Edgett, Kenneth S. (2002). "Low-albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks". Journal of Geophysical Research 107: 5038. Bibcode 2002JGRE..107.5038E. doi:10.1029/2001JE001587. 
  16. ^ Lemmon, Mt; Wolff, Mj; Smith, Md; Clancy, Rt; Banfield, D; Landis, Ga; Ghosh, A; Smith, Ph; Spanovich, N; Whitney, B; Whelley, P; Greeley, R; Thompson, S; Bell, Jf, 3Rd; Squyres, Sw (Dec 2004). "Atmospheric imaging results from the Mars exploration rovers: Spirit and Opportunity". Science 306 (5702): 1753–6. Bibcode 2004Sci...306.1753L. doi:10.1126/science.1104474. ISSN 0036-8075. PMID 15576613. 

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