Carbonates on Mars
![](http://178.128.105.246/cars-http-upload.wikimedia.org/wikipedia/commons/thumb/5/5a/PIA19816-Mars-EstimatingCarbon-Orbiters-20150902.jpg/400px-PIA19816-Mars-EstimatingCarbon-Orbiters-20150902.jpg)
The formation of carbonates on Mars have been suggested based on evidence of the presence of liquid water and atmospheric carbon dioxide in the planet's early stages.[1] Moreover, due to their utility in registering changes in environmental conditions such as pH, temperature, fluid composition,[2] carbonates have been considered as a primary target for planetary scientists' research.[1] However, since their first detection in 2008,[3] the large deposits of carbonates that were one expected on Mars have not been found,[4] leading to multiple potential explanations that can explain why carbonates did not form massively on the planet.
Mars probes
[edit]Previously, most remote sensing instruments such as OMEGA and THEMIS—sensitive to infrared emissivity spectral features of carbonates—had not suggested the presence of carbonate outcrops,[5] at least at the 100 m or coarser spatial scales available from the returned data.[6]
Though ubiquitous, a 2003 study of carbonates on Mars showed that they are dominated by magnesite (MgCO3) in Martian dust, had mass fractions less than 5%, and could have formed under current atmospheric conditions.[7] Furthermore, with the exception of the surface dust component, by 2007 carbonates had not been detected by any in situ mission, even though mineralogic modeling did not preclude small amounts of calcium carbonate in Independence class rocks of Husband Hill in Gusev crater.[8][9] (note: An IAU naming convention within Gusev is not yet established).
Remote sensing data
[edit]The first successful identification of a strong infrared spectral signature from surficial carbonate minerals of local scale (< 10 km2) was made by the MRO-CRISM team in 2008.[10] Spectral modeling in 2007 identified a key deposit in Nili Fossae dominated by a single mineral phase that was spatially associated with olivine outcrops. The dominant mineral appeared to be magnesite, while morphology inferred with HiRISE and thermal properties suggested that the deposit was lithic. Stratigraphically, this layer appeared between phyllosilicates below and mafic cap rocks above, temporally between the Noachian and Hesperian eras. Even though infrared spectra are representative of minerals to less than ≈0.1 mm depths[11] (in contrast to gamma spectra which are sensitive to tens of cm depths),[12] stratigraphic,[clarification needed] morphologic,[clarification needed] and thermal properties are consistent with the existence of the carbonate as outcrop rather than alteration rinds.[clarification needed] Nevertheless, the morphology was distinct from typical terrestrial sedimentary carbonate layers suggesting formation from local aqueous alteration of olivine and other igneous minerals. However, key implications were that the alteration would have occurred under moderate pH and that the resulting carbonates were not exposed to sustained low pH aqueous conditions even as recently as the Hesperian.
Evidence for widespread presence of carbonates began to increase in 2009, when low levels (<10%) of Mg-rich carbonates were found across the Martian area of Syrtis Major, Margaritifer Terra, Lunae Planum, Elysium Planitia, as reported from analysis of data acquired by the Planetary Fourier Spectrometer (PFS) on board the Mars Express spacecraft.[13]
when the Thermal and Evolved Gas Analyzer (TEGA) and WCL experiments on the 2009 Phoenix Mars lander found between 3–5wt% calcite (CaCO3) and an alkaline soil.[14] In 2010 analyses by the Mars Exploration Rover Spirit, identified outcrops rich in magnesium-iron carbonate (16–34 wt%) in the Columbia Hills of Gusev crater, most likely precipitated from carbonate-bearing solutions under hydrothermal conditions at near-neutral pH in association with volcanic activity during the Noachian era.[15]
After Spirit Rover stopped working scientists studied old data from the Miniature Thermal Emission Spectrometer, or Mini-TES and confirmed the presence of large amounts of carbonate-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][15]
Carbonates (calcium or iron carbonates) were discovered in a crater on the rim of Huygens Crater, located in the Iapygia quadrangle. The impact on the rim exposed material that had been dug up from the impact that created Huygens. These minerals represent evidence that Mars once had a thicker carbon dioxide atmosphere with abundant moisture. These kind of carbonates only form when there is a lot of water. They were found with the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument on the Mars Reconnaissance Orbiter. Earlier, the instrument had detected clay minerals. The carbonates were found near the clay minerals. Both of these minerals form in wet environments. It is supposed that billions of years age Mars was much warmer and wetter. At that time, carbonates would have formed from water and the carbon dioxide-rich atmosphere. Later the deposits of carbonate would have been buried. The double impact has now exposed the minerals. Earth has vast carbonate deposits in the form of limestone.[17]
Name | Mission | ||
---|---|---|---|
MgCO3 | magnesite | remote sensing, MRO-CRISM | 2008 |
MgCO3 | magnesite | remote sensing Mars Express-PFS | 2009 |
CaCO3 | calcite | Phoenix | 2009 |
FeCO3 | siderite | Curiosity | 2020 |
Absence of Carbonates on Mars
[edit]Geological and geomorphological evidence has reinforced the idea of the presence of liquid water on early Mars.[4][18] Therefore, abundant precipitation of carbonates from atmospheric and water reactions is expected. However, spectral imaging has revealed only small amounts of carbonates, generating doubts about humans' understanding of geological processes on Mars.[4] To overcome this problem, scientists have proposed explanations that reconcile the absence of carbonates with the presence of a CO2-rich atmosphere and liquid water.
Cold and Dry Early Mars Environments
[edit]According to this explanation, the early Martian conditions are similar to those at present.[19] Essentially, it suggests that carbonates are absent because the planet never experienced conditions that included the presence of liquid water and a CO2-rich thick atmosphere. Even if this explanation provides an insight in the reasons why carbonates are not present, it is in disagreement with the geomorphological and mineralogical evidence supporting the existence of liquid water on Mars' surface.[1][4][18]
Inability of Detection with Current Technology
[edit]This hypothesis establishes that the Thermal Emission Spectrometer (TES) aboard the Mars Global Surveyor spacecraft and the Thermal Emission Imaging System (THEMIS) on board the Mars Odyssey spacecraft are unable to detect carbonates.[20] According to this notion, the carbonates indeed formed and are still exist on Mars, but they remain undetected due to the limited sensitivity of the current tools used for mineralogical detection on the planet.[20]
Secondary Chemical Alteration
[edit]This concept involves the potential for secondary chemical alteration of ancient carbonates on Mars, due to the formation of acid rain[21] resulting from the combination of water vapor and sulfates. The consequence of this process implies the chemical decomposition of superficial carbonates layers, as carbonates are not resistant to acidic pH conditions; acid-fog weathering; and photo-decomposition.[22][23]
Hidden Carbonate Deposits
[edit]According to this perspective, massive carbonates deposits formed but are hidden beneath several layers of secondary alteration rocks, preventing their identification on the surface. Other alternatives to this hypothesis include: Masking of carbonates as a consequence of the abundant soils on Mars; and resurfacing processes that have covered carbonate deposits, such as eolian deposition and late sedimentation processes.[24]
Inhibition due to Acidic Conditions
[edit]Finally, this hypothesis defends the idea that carbonates never precipitated because the pH conditions of the environment were too acidic to allow carbonates to precipitate, or at least siderite, which is the primary carbonate mineral expected to precipitate first.[25] The acidic conditions are derived from the high partial pressures of atmospheric carbon dioxide, as well as a persistent sulfate and iron enrichment that affect the optimal conditions for carbonates to precipitate.[4]
Gallery
[edit]-
Huygens Crater - circle shows location of carbonate deposit - representing a time when Mars had abundant liquid water on its surface (Scale bar = 259 km).
-
Nili Fossae on Mars - largest known carbonate deposit.
See also
[edit]- Areography (geography of Mars)
- Chemical gardening – Demonstration of metallic salts crystallization
- Chloride-bearing deposits on Mars
- Composition of Mars
- Elysium Planitia
- Fretted terrain
- Geology of Mars
- Glaciers on Mars
- Gravity of Mars
- Groundwater on Mars
- Hecates Tholus
- Iapygia quadrangle
- Lakes on Mars
- Life on Mars
- List of quadrangles on Mars
- List of rocks on Mars
- Magnetic field of Mars
- Mars Geyser Hopper
- Martian craters
- Martian dichotomy
- Martian geyser
- Martian gullies
- Martian soil
- Mineralogy of Mars
- Ore resources on Mars
- Scientific information from the Mars Exploration Rover mission
- Seasonal flows on warm Martian slopes
- Vallis
- Water on Mars
- Mars carbonate catastrophe
References
[edit]- ^ a b c Niles, Paul B.; Catling, David C.; Berger, Gilles; Chassefière, Eric; Ehlmann, Bethany L.; Michalski, Joseph R.; Morris, Richard; Ruff, Steven W.; Sutter, Brad (January 2013). "Geochemistry of Carbonates on Mars: Implications for Climate History and Nature of Aqueous Environments". Space Science Reviews. 174 (1–4): 301–328. Bibcode:2013SSRv..174..301N. doi:10.1007/s11214-012-9940-y. ISSN 0038-6308.
- ^ Bridges, John C.; Hicks, Leon J.; Treiman, Allan H. (2019-01-01), Filiberto, Justin; Schwenzer, Susanne P. (eds.), "Chapter 5 - Carbonates on Mars", Volatiles in the Martian Crust, Elsevier, pp. 89–118, doi:10.1016/b978-0-12-804191-8.00005-2, ISBN 978-0-12-804191-8, retrieved 2024-04-30
- ^ Ehlmann, Bethany L.; Mustard, John F.; Murchie, Scott L.; Poulet, Francois; Bishop, Janice L.; Brown, Adrian J.; Calvin, Wendy M.; Clark, Roger N.; Marais, David J. Des; Milliken, Ralph E.; Roach, Leah H.; Roush, Ted L.; Swayze, Gregg A.; Wray, James J. (19 December 2008). "Orbital Identification of Carbonate-Bearing Rocks on Mars". Science. 322 (5909): 1828–1832. Bibcode:2008Sci...322.1828E. doi:10.1126/science.1164759. PMID 19095939. S2CID 1190585.
- ^ a b c d e Fairén, Alberto G.; Fernández-Remolar, David; Dohm, James M.; Baker, Victor R.; Amils, Ricardo (September 2004). "Inhibition of carbonate synthesis in acidic oceans on early Mars". Nature. 431 (7007): 423–426. Bibcode:2004Natur.431..423F. doi:10.1038/nature02911. ISSN 1476-4687. PMID 15386004.
- ^ Bibring, Jean-Pierre; Langevin, Yves; Mustard, John F.; Poulet, François; Arvidson, Raymond; Gendrin, Aline; Gondet, Brigitte; Mangold, Nicolas; Pinet, P.; Forget, F.; Berthé, Michel; Bibring, Jean-Pierre; Gendrin, Aline; Gomez, Cécile; Gondet, Brigitte; Jouglet, Denis; Poulet, François; Soufflot, Alain; Vincendon, Mathieu; Combes, Michel; Drossart, Pierre; Encrenaz, Thérèse; Fouchet, Thierry; Merchiorri, Riccardo; Belluci, GianCarlo; Altieri, Francesca; Formisano, Vittorio; Capaccioni, Fabricio; Cerroni, Pricilla; Coradini, Angioletta; Fonti, Sergio; Korablev, Oleg; Kottsov, Volodia; Ignatiev, Nikolai; Moroz, Vassili; Titov, Dimitri; Zasova, Ludmilla; Loiseau, Damien; Mangold, Nicolas; Pinet, Patrick; Douté, Sylvain; Schmitt, Bernard; Sotin, Christophe; Hauber, Ernst; Hoffmann, Harald; Jaumann, Ralf; Keller, Uwe; Arvidson, Ray; Mustard, John F.; Duxbury, Tom; Forget, François; Neukum, G. (21 April 2006). "Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data". Science. 312 (5772): 400–404. Bibcode:2006Sci...312..400B. doi:10.1126/science.1122659. PMID 16627738. S2CID 13968348.
- ^ Catling, David C. (July 2007). "Ancient fingerprints in the clay". Nature. 448 (7149): 31–32. doi:10.1038/448031a. PMID 17611529. S2CID 4387261.
- ^ Bandfield, Joshua L.; Glotch, Timothy D.; Christensen, Philip R. (22 August 2003). "Spectroscopic Identification of Carbonate Minerals in the Martian Dust". Science. 301 (5636): 1084–1087. Bibcode:2003Sci...301.1084B. doi:10.1126/science.1088054. PMID 12934004. S2CID 38721436.
- ^ Tarnas, J. D.; Stack, K. M.; Parente, M.; Koeppel, A. H. D.; Mustard, J. F.; Moore, K. R.; Horgan, B. H. N.; Seelos, F. P.; Cloutis, E. A.; Kelemen, P. B.; Flannery, D.; Brown, A. J.; Frizzell, K. R.; Pinet, P. (November 2021). "Characteristics, Origins, and Biosignature Preservation Potential of Carbonate-Bearing Rocks Within and Outside of Jezero Crater". Journal of Geophysical Research: Planets. 126 (11): e2021JE006898. Bibcode:2021JGRE..12606898T. doi:10.1029/2021JE006898. PMC 8597593. PMID 34824965.
- ^ Clark, B. C.; Arvidson, R. E.; Gellert, R.; Morris, R. V.; Ming, D. W.; Richter, L.; Ruff, S. W.; Michalski, J. R.; Farrand, W. H.; Yen, A.; Herkenhoff, K. E.; Li, R.; Squyres, S. W.; Schröder, C.; Klingelhöfer, G.; Bell, J. F. (June 2007). "Evidence for montmorillonite or its compositional equivalent in Columbia Hills, Mars". Journal of Geophysical Research: Planets. 112 (E6). Bibcode:2007JGRE..112.6S01C. doi:10.1029/2006JE002756.
- ^ Ehlmann, Bethany L.; Mustard, John F.; Murchie, Scott L.; Poulet, Francois; Bishop, Janice L.; Brown, Adrian J.; Calvin, Wendy M.; Clark, Roger N.; Marais, David J. Des; Milliken, Ralph E.; Roach, Leah H.; Roush, Ted L.; Swayze, Gregg A.; Wray, James J. (19 December 2008). "Orbital Identification of Carbonate-Bearing Rocks on Mars". Science. 322 (5909): 1828–1832. Bibcode:2008Sci...322.1828E. doi:10.1126/science.1164759. PMID 19095939. S2CID 1190585.
- ^ Poulet, F.; Gomez, C.; Bibring, J.-P.; Langevin, Y.; Gondet, B.; Pinet, P.; Belluci, G.; Mustard, J. (August 2007). "Martian surface mineralogy from Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité on board the Mars Express spacecraft (OMEGA/MEx): Global mineral maps" (PDF). Journal of Geophysical Research: Planets. 112 (E8). Bibcode:2007JGRE..112.8S02P. doi:10.1029/2006JE002840.
- ^ Boynton, W. V.; Taylor, G. J.; Evans, L. G.; Reedy, R. C.; Starr, R.; Janes, D. M.; Kerry, K. E.; Drake, D. M.; Kim, K. J.; Williams, R. M. S.; Crombie, M. K.; Dohm, J. M.; Baker, V.; Metzger, A. E.; Karunatillake, S.; Keller, J. M.; Newsom, H. E.; Arnold, J. R.; Brückner, J.; Englert, P. A. J.; Gasnault, O.; Sprague, A. L.; Mitrofanov, I.; Squyres, S. W.; Trombka, J. I.; d'Uston, L.; Wänke, H.; Hamara, D. K. (December 2007). "Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars". Journal of Geophysical Research: Planets. 112 (E12). Bibcode:2007JGRE..11212S99B. doi:10.1029/2007JE002887.
- ^ Palomba, Ernesto; Zinzi, Angelo; Cloutis, Edward A.; D’Amore, Mario; Grassi, Davide; Maturilli, Alessandro (September 2009). "Evidence for Mg-rich carbonates on Mars from a 3.9 μm absorption feature" (PDF). Icarus. 203 (1): 58–65. Bibcode:2009Icar..203...58P. doi:10.1016/j.icarus.2009.04.013. S2CID 121348711.
- ^ Boynton, W. V.; Ming, D. W.; Kounaves, S. P.; Young, S. M. M.; Arvidson, R. E.; Hecht, M. H.; Hoffman, J.; Niles, P. B.; Hamara, D. K.; Quinn, R. C.; Smith, P. H.; Sutter, B.; Catling, D. C.; Morris, R. V. (3 July 2009). "Evidence for Calcium Carbonate at the Mars Phoenix Landing Site". Science. 325 (5936): 61–64. Bibcode:2009Sci...325...61B. doi:10.1126/science.1172768. PMID 19574384. S2CID 26740165.
- ^ a b Morris, Richard V.; Ruff, Steven W.; Gellert, Ralf; Ming, Douglas W.; Arvidson, Raymond E.; Clark, Benton C.; Golden, D. C.; Siebach, Kirsten; Klingelhöfer, Göstar; Schröder, Christian; Fleischer, Iris; Yen, Albert S.; Squyres, Steven W. (23 July 2010). "Identification of Carbonate-Rich Outcrops on Mars by the Spirit Rover". Science. 329 (5990): 421–424. Bibcode:2010Sci...329..421M. doi:10.1126/science.1189667. PMID 20522738.
- ^ "Outcrop of long-sought rare rock on Mars found". ScienceDaily (Press release). Arizona State University. 4 June 2010.
- ^ "Some of Mars' Missing Carbon Dioxide May be Buried". NASA/JPL. Archived from the original on 2011-12-05.
- ^ a b Wordsworth, Robin D. (2016-06-29). "The Climate of Early Mars". Annual Review of Earth and Planetary Sciences. 44 (1): 381–408. arXiv:1606.02813. Bibcode:2016AREPS..44..381W. doi:10.1146/annurev-earth-060115-012355. ISSN 0084-6597.
- ^ Carr, Michael H.; Head, James W. (May 2003). "Oceans on Mars: An assessment of the observational evidence and possible fate". Journal of Geophysical Research: Planets. 108 (E5). Bibcode:2003JGRE..108.5042C. doi:10.1029/2002JE001963. ISSN 0148-0227.
- ^ a b Kirkland, Laurel E.; Herr, Kenneth C.; Adams, Paul M. (December 2003). "Infrared stealthy surfaces: Why TES and THEMIS may miss some substantial mineral deposits on Mars and implications for remote sensing of planetary surfaces". Journal of Geophysical Research: Planets. 108 (E12): 5137. Bibcode:2003JGRE..108.5137K. doi:10.1029/2003JE002105. ISSN 0148-0227.
- ^ Craddock, Robert A.; Howard, Alan D. (November 2002). "The case for rainfall on a warm, wet early Mars". Journal of Geophysical Research: Planets. 107 (E11). Bibcode:2002JGRE..107.5111C. doi:10.1029/2001JE001505. ISSN 0148-0227.
- ^ Huguenin, Robert L. (1974-09-10). "The formation of goethite and hydrated clay minerals on Mars". Journal of Geophysical Research. 79 (26): 3895–3905. Bibcode:1974JGR....79.3895H. doi:10.1029/JB079i026p03895.
- ^ Mukhin, L. M.; Koscheevi, A. P.; Dikov, Yu P.; Huth, J.; Wänke, H. (January 1996). "Experimental simulations of the photodecomposition of carbonates and sulphates on Mars". Nature. 379 (6561): 141–143. Bibcode:1996Natur.379..141M. doi:10.1038/379141a0. ISSN 1476-4687. PMID 8538763.
- ^ Baker, Victor R. (July 2001). "Water and the martian landscape". Nature. 412 (6843): 228–236. Bibcode:2001Natur.412..228B. doi:10.1038/35084172. ISSN 1476-4687. PMID 11449284.
- ^ Catling, David C. (1999-07-25). "A chemical model for evaporites on early Mars: Possible sedimentary tracers of the early climate and implications for exploration". Journal of Geophysical Research: Planets. 104 (E7): 16453–16469. Bibcode:1999JGR...10416453C. doi:10.1029/1998JE001020. ISSN 0148-0227.