Martian meteorite

Martian meteorite (SNC meteorites)
— Clan —

Martian meteorite EETA79001, shergottite
Type Achondrite
Subgroups
Parent body Mars
Total known specimens 132 as of 9 March 2014 [1]

Martian meteorite NWA 7034, nicknamed "Black Beauty," weighs approximately 320 g (11 oz).[2]

A Martian meteorite is a rock that formed on the planet Mars and was then ejected from Mars by the impact of an asteroid or comet, and finally landed on the Earth. Of over 61,000 meteorites that have been found on Earth, 132 were identified as Martian as of 3 March 2014.[1] These meteorites are thought to be from Mars because they have elemental and isotopic compositions that are similar to rocks and atmosphere gases analyzed by spacecraft on Mars.[3] On October 17, 2013, NASA reported, based on analysis of argon in the Martian atmosphere by the Mars Curiosity rover, that certain meteorites found on Earth thought to be from Mars were indeed from Mars.[4]

The term does not refer to meteorites found on Mars, such as Heat Shield Rock.

On January 3, 2013, NASA reported that a meteorite, named NWA 7034 (nicknamed "Black Beauty"), found in 2011 in the Sahara desert, was determined to be from Mars and found to contain ten times the water of other Mars meteorites found on Earth.[2] The meteorite was determined to have formed 2.1 billion years ago during the Amazonian geologic period on Mars.

History

By the early 1980s, it was obvious that the SNC group of meteorites (Shergottites, Nakhlites, Chassignites) were significantly different from most other meteorite types. Among these differences were younger formation ages, a different oxygen isotopic composition, the presence of aqueous weathering products, and some similarity in chemical composition to analyses of the Martian surface rocks in 1976 by the Viking landers. Several scientists suggested these characteristics implied the origin of SNC meteorites from a relatively large parent body, possibly Mars (e.g., Smith et al.[5] and Treiman et al.[6]). Then in 1983, various trapped gases were reported in impact-formed glass of the EET79001 shergottite, gases which closely resembled those in the Martian atmosphere as analyzed by Viking.[7] These trapped gases provided direct evidence for a Martian origin. In 2000, an article by Treiman, Gleason and Bogard gave a survey of all the arguments used to conclude the SNC meteorites (of which 14 had been found at the time) were from Mars. They wrote, "There seems little likelihood that the SNCs are not from Mars. If they were from another planetary body, it would have to be substantially identical to Mars as it now is understood."[3]

Subdivision

The Martian meteorites are divided into 3 groups (orange) and two grouplets (yellow). SHE = Shergottite, NAK = Nakhlite, CHA = Chassignite, OPX = Orthopyroxenite (ALH 84001), BBR = Basaltic Breccia (NWA 7034).

As of January 9, 2013, 111 of the 114 Martian meteorites are divided into three rare groups of achondritic (stony) meteorites: shergottites (96), nakhlites (13), chassignites (2), and ones otherwise (3) (which includes the oddball meteorite Allan Hills 84001 usually placed within a specific "OPX group").[1] Consequently, Martian meteorites as a whole are sometimes referred to as the SNC group. They have isotope ratios that are said to be consistent with each other and inconsistent with the Earth. The names derive from the location of where the first meteorite of their type was discovered.

Shergottites

Roughly three-quarters of all Martian meteorites can be classified as shergottites. They are named after the Shergotty meteorite, which fell at Sherghati, India in 1865.[8] Shergottites are igneous rocks of mafic to ultramafic lithology. They fall into three main groups, the basaltic, olivine-phyric (such as the Tissint group found in Morocco in 2011[9][10]) and lherzolitic shergottites, based on their crystal size and mineral content. They can be categorised alternatively into three or four groups based on their rare-earth element content.[11] These two classification systems do not line up with each other, hinting at complex relationships between the various source rocks and magmas that the shergottites formed from.

NWA 6963,[12] a shergottite found in Morocco, September 2011.

The shergottites appear to have crystallised as recently as 180 million years ago,[13] which is a surprisingly young age considering how ancient the majority of the surface of Mars appears to be, and the small size of Mars itself. Because of this, some have advocated the idea that the shergottites are much older than this.[14] This "Shergottite Age Paradox" remains unsolved and is still an area of active research and debate.

The 3-million-year-old crater Mojave, 58.5 km in diameter and the youngest crater of its size on the planet, has been identified as a potential source of these meteorites.[15]

Nakhlites

Nakhla meteorite's two sides and its inner surfaces after breaking it in 1998

Nakhlites are named after the first of them, the Nakhla meteorite, which fell in El-Nakhla, Alexandria, Egypt in 1911 and had an estimated weight of 10 kg.

Nakhlites are igneous rocks that are rich in augite and were formed from basaltic magma about 1.3 billion years ago. They contain augite and olivine crystals. Their crystallization ages, compared to a crater count chronology of different regions on Mars, suggest the nakhlites formed on the large volcanic construct of either Tharsis, Elysium, or Syrtis Major Planum.[16]

It has been shown that the nakhlites were suffused with liquid water around 620 million years ago and that they were ejected from Mars around 10.75 million years ago by an asteroid impact. They fell to Earth within the last 10,000 years.[16]

Chassignites

The first chassignite, the Chassigny meteorite, fell at Chassigny, Haute-Marne, France in 1815. There has been only one other chassignite recovered, named Northwest Africa (NWA) 2737. NWA 2737 was found in Morocco or Western Sahara in August 2000 by meteorite hunters Bruno Fectay and Carine Bidaut, who gave it the temporary name "Diderot." It was shown by Beck et al.[17] that its "mineralogy, major and trace element chemistry as well as oxygen isotopes revealed an unambiguous Martian origin and strong affinities with Chassigny."

Ungrouped meteorites

Allan Hills 84001 (ALH 84001)

Among these, the famous specimen Allan Hills 84001 has a different rock type than other Martian meteorites: it is an orthopyroxenite (an igneous rock dominantly composed of orthopyroxene). For this reason it is classified within its own group, the "OPX Martian meteorites". This meteorite received much attention after an electron microscope revealed structures that were considered to be the fossilized remains of bacteria-like lifeforms. As of 2005, scientific consensus was that the microfossils were not indicative of Martian life, but of contamination by earthly biofilms. ALH 84001 is as old as the basaltic and intermediate shergottite groups — i.e., 4.1 billion years old.

In March 2004 it was suggested that the unique Kaidun meteorite, which landed in Yemen on March 12, 1980, may have originated on the Martian moon of Phobos.[18] Because Phobos has similarities to C-type asteroids and because the Kaidun meteorite is a carbonaceous chondrite, Kaidun is not a Martian meteorite in the strict sense. However, it may contain small fragments of material from the Martian surface.

Origin

The majority of SNC meteorites are quite young compared to most other meteorites and seem to imply that volcanic activity was present on Mars only a few hundred million years ago. The young formation ages of Martian meteorites was one of the early recognized characteristics that suggested their origin from a planetary body such as Mars. Among Martian meteorites, only ALH 84001 and NWA 7034 have radiometric ages older than about 1400 Ma (Ma = million years). All nakhlites, as well as Chassigny and NWA 2737, give similar if not identical formation ages around 1300 Ma, as determined by various radiometric dating techniques.[13][19] Formation ages determined for many shergottites are variable and much younger, mostly ~150-575 Ma.[13][20][21][22] The chronological history of shergottites is not totally understood, and a few scientists have suggested that some may actually have formed prior to the times given by their radiometric ages,[23] a suggestion not accepted by most scientists. Formation ages of SNC meteorites are often linked to their cosmic-ray exposure (CRE) ages, as measured from the nuclear products of interactions of the meteorite in space with energetic cosmic ray particles. Thus, all measured nakhlites give essentially identical CRE ages of approximately 11 Ma, which when combined with their possible identical formation ages indicates ejection of nakhlites into space from a single location on Mars by a single impact event.[13] Some of the shergottites also seem to form distinct groups according to their CRE ages and formation ages, again indicating ejection of several different shergottites from Mars by a single impact. However, CRE ages of shergottites vary considerably (~0.5-19 Ma),[13] and several impact events are required to eject all the known shergottites. It had been asserted that there are no large young craters on Mars that are candidates as sources for the Martian meteorites, but subsequent studies claimed to have a likely source for ALH 84001[24] and a possible source for other shergottites.[25]

In a 2014 paper, several researchers claimed that all shergottites meteorites come from the Mojave Crater on Mars.[26]

Age estimates based on cosmic ray exposure

The amount of time spent in transit from Mars to Earth can be estimated by measurements of the effect of cosmic radiation on the meteorites, particularly on isotope ratios of noble gases. The meteorites cluster in families that seem to correspond to distinct impact events on Mars.

It is thought, therefore, that the meteorites all originate in relatively few impacts every few million years on Mars. The impactors would be kilometers in diameter and the craters they form on Mars tens of kilometers in diameter. Models of impacts on Mars are consistent with these findings.[27]

Ages since impact determined so far include[28][29]

Type Age (mya)
Dhofar 019, olivine-phyric shergottite 19.8 ± 2.3[27]
ALH 84001, orthopyroxenite15.0 ± 0.8[27]
dunite (Chassigny) 11.1 ± 1.6 [27]
Five nakhlites 10.6 ± 1.0 [27]
Lherzolites 3.8–4.7[27]
six basaltic shergottites 2.4–3.0[27]
Five olivine-phyric shergottites 1.2 ± 0.1[27]
EET 79001 0.73 ± 0.15[27]

Possible evidence of life

Several Martian meteorites have been found to contain what some think is evidence for fossilized Martian life forms. The most significant of these is a meteorite found in the Allan Hills of Antarctica (ALH 84001). Ejection from Mars seems to have taken place about 16 million years ago. Arrival on Earth was about 13 000 years ago. Cracks in the rock appear to have filled with carbonate materials (implying groundwater was present) between 4 and 3.6 billion-years-ago. Evidence of polycyclic aromatic hydrocarbons (PAHs) have been identified with the levels increasing away from the surface. Other Antarctic meteorites do not contain PAHs. Earthly contamination should presumably be highest at the surface. Several minerals in the crack fill are deposited in phases, specifically, iron deposited as magnetite, that are claimed to be typical of biodepositation on Earth. There are also small ovoid and tubular structures that might be nanobacteria fossils in carbonate material in crack fills (investigators McKay, Gibson, Thomas-Keprta, Zare).[30] Micropaleontologist Schopf, who described several important terrestrial bacterial assemblages, examined ALH 84001 and opined that the structures are too small to be Earthly bacteria and don't look especially like lifeforms to him. The size of the objects is consistent with Earthly "nanobacteria", but the existence of nanobacteria itself is controversial.

Many studies disputed the validity of the fossils.[31][32] For example, it was found that most of the organic matter in the meteorite was of terrestrial origin.[33] But, a recent study suggests that magnetite in the meteorite could have been produced by Martian microbes. The study, published in the journal of the Geochemical and Meteoritic Society, used more advanced high resolution electron microscopy than was possible in 1996.[34] A serious difficulty with the claims for a biogenic origin of the magnetites is that the majority of them exhibit topotactic crystallographic relationships with the host carbonates (i.e. there are 3D orientation relationships between the magnetite and carbonate lattices), which is strongly indicative that the magnetites have grown in situ by a physico-chemical mechanism.[35]

While water is no indication of life many of the meteorites found on Earth have shown water including NWA 7034 which is a more rare meteorite from the Amazonian period of Martian history.[36] Water has since been found on the surface of Mars in the form of recurring slope lineae and further supports the earlier evidence provided by martian meteorites. The water is likely too minimal to support life. [37]

See also

References

  1. 1 2 3 Meteoritical Bulletin Database
  2. 1 2 Staff (January 3, 2013). "Researchers Identify Water Rich Meteorite Linked To Mars Crust". NASA. Retrieved January 3, 2013.
  3. 1 2 Treiman, A.H.; et al. (October 2000). "The SNC meteorites are from Mars". Planetary and Space Science. 48 (12–14): 1213–1230. Bibcode:2000P&SS...48.1213T. doi:10.1016/S0032-0633(00)00105-7.
  4. ↑ Webster, Guy (October 17, 2013). "NASA Rover Confirms Mars Origin of Some Meteorites". NASA. Retrieved October 29, 2013.
  5. ↑ Smith, M.R.; Laul, J. C.; Ma, M. S.; Huston, T.; Verkouteren, R. M.; Lipschutz, M. E.; Schmitt, R. A. (February 15, 1984). "Petrogenesis of the SNC (Shergottites, Nakhlites, Chassignites) Meteorites: Implications for Their Origin From a Large Dynamic Planet, Possibly Mars.". Journal of Geophysical Research. 89 (S02): B612–B630. Bibcode:1984JGRS...89..612S. doi:10.1029/JB089iS02p0B612.
  6. ↑ Allan H. Treiman; Michael J. Drake; Marie-Josee Janssens; Rainer Wolf; Mitsuru Ebihara (January 1986). "Core formation in the Earth and Shergottite Parent Body (SPB):Chemical evidence from basalts". Geochimica et Cosnochimica Acta. 50 (6): 1071–1091. doi:10.1016/0016-7037(86)90389-3. (Subscription required (help)).
  7. ↑ Bogard, D. D.; Johnson, P. (1983). "Martian gases in an Antarctic meteorite". Science. 221 (4611): 651–654. Bibcode:1983Sci...221..651B. PMID 17787734. doi:10.1126/science.221.4611.651.
  8. ↑ Shergotty Meteorite - JPL, NASA
  9. ↑
  10. ↑ Morin, Monte (October 12, 2012). "An unusually pristine piece of Mars". Los Angeles Times.
  11. ↑ The SNC meteorites: basaltic igneous processes on Mars, Bridges & Warren 2006
  12. ↑ NWA 6963
  13. 1 2 3 4 5 Nyquist, L.E.; et al. (2001). "Ages and geologic histories of martian meteorites". Space Science Reviews. 96: 105–164. Bibcode:2001SSRv...96..105N. doi:10.1023/A:1011993105172.
  14. ↑ Bouvier, A. et al., 2009. Martian meteorite chronology and the evolution of the interior of Mars. Earth and Planetary Science Letters Volume 280, pp. 285-295. " doi:10.1016/j.epsl.2009.01.042
  15. ↑ Werner, S. C.; Ody, A.; Poulet, F. (2014-03-06). "The Source Crater of Martian Shergottite Meteorites". Science. 343: 1343–6. PMID 24603150. doi:10.1126/science.1247282.
  16. 1 2 Treiman, A.H., "The nakhlite meteorites: Augite-rich igneous rocks from Mars" - (PDF) Chemie der Erde 65, p. 203-270, (2005). URL accessed July 30, 2011.
  17. ↑ Beck, P.; et al. (March 14–18, 2005). The Diderot meteorite: The second chassignite (PDF). 36th Annual Lunar and Planetary Science Conference. League City, Texas. abstract no.1326. Retrieved September 8, 2006.
  18. ↑ Zolensky, M. and Ivanov A. (2003). "The Kaidun Microbreccia Meteorite: A Harvest from the Inner and Outer Asteroid Belt". Chemie der Erde/Geochemistry. 63 (3): 185–246. Bibcode:2003ChEG...63..185Z. doi:10.1078/0009-2819-00038. Retrieved 2008-11-26.
  19. ↑ Park, J.; et al. (2009). "39Ar-40Ar ages of martian nakhlites". Geochim. Cosmochim. Acta. 73 (7): 2177–2189. Bibcode:2009GeCoA..73.2177P. doi:10.1016/j.gca.2008.12.027.
  20. ↑ Borg, L.E.; et al. (2005). "Constraints on the U-Pbisotopic systematics of Mars inferred from a combined U-Pb, Rb-Sr, and Sm-Nd isotopic study of the martian meteorite Zagami". Geochim. Cosmochim. Acta. 69 (24): 5819–5830. Bibcode:2005GeCoA..69.5819B. doi:10.1016/j.gca.2005.08.007.
  21. ↑ Shih, C-Y; et al. (2005). "Rb-Sr and Sm-Nd dating of olivine-phyric shergottite Yamato 980459: Petrogenesis of depleted shergottites". Antarctic Meteorite Research. 18: 46–65. Bibcode:2005AMR....18...46S.
  22. ↑ Nyquist, L.E.; et al. (2009). "Concordant Rb-Sr, Sm-Nd, and Ar-Ar ages for Northwest Africa 1460: A 446 Ma old basaltic shergottite related to "lherzolitic" shergottites". Geochim. Cosmochim. Acta. 73 (14): 4288–4309. Bibcode:2009GeCoA..73.4288N. doi:10.1016/j.gca.2009.04.008.
  23. ↑ Bouvier, A.; et al. (2008). "The case for old basaltic shergottites". Earth Planet. Sci. Lett. 266: 105–124. Bibcode:2008E&PSL.266..105B. doi:10.1016/j.epsl.2007.11.006.
  24. ↑ "Birthplace of famous Mars meteorite pinpointed" - September 16, 2005 New Scientist article. URL accessed September 8, 2006.
  25. ↑ McEwen, A.S.; Preblich, B; Turtle, E; Artemieva, N; Golombek, M; Hurst, M; Kirk, R; Burr, D; Christensen, P (2005). "The rayed crater Zunil and interpretations of small impact craters on Mars" (PDF). Icarus. 176 (2): 351–381. Bibcode:2005Icar..176..351M. doi:10.1016/j.icarus.2005.02.009. Retrieved 2006-09-08..
  26. ↑ http://www.sciencemag.org/content/early/2014/03/05/science.1247282
  27. 1 2 3 4 5 6 7 8 9 O. Eugster, G. F. Herzog, K. Marti, M. W. Caffee Irradiation Records, Cosmic-Ray Exposure Ages, and Transfer Times of Meteorites, see section 4.5 Martian Meteorites LPI, 2006
  28. ↑ L.E. NYQUIST1, D.D. BOGARD1, C.-Y. SHIH2, A. GRESHAKE3, D. STÖFFLER AGES AND GEOLOGIC HISTORIES OF MARTIAN METEORITES 2001
  29. ↑ Tony Irving Martian Meteorites - has graphs of ejection ages - site maintained by Tony Irving for up to date information on Martian meteorites
  30. ↑ McKay, D.; Gibson Jr, EK; Thomas-Keprta, KL; Vali, H; Romanek, CS; Clemett, SJ; Chillier, XD; Maechling, CR; Zare, RN (1996). "Search for Past Life on Mars: Possible Relic Biogenic Activity in Martian Meteorite AL84001". Science. 273 (5277): 924–930. Bibcode:1996Sci...273..924M. PMID 8688069. doi:10.1126/science.273.5277.924.
  31. ↑ Gibbs, W. and C. Powell. In Focus Bugs in the Data? 1996. Scientific American. October. 20-22
  32. ↑ Controversy Continues: Mars Meteorite Clings to Life - Or Does It? By Leonard David - Senior Space Writer, posted: 20 March 2002, Space.com
  33. ↑ Bada, J. L.; Glavin, DP; McDonald, GD; Becker, L (1998). "A Search for Endogenous Amino Acids in Martian Meteorite ALH84001". Science. 279 (5349): 362–5. Bibcode:1998Sci...279..362B. PMID 9430583. doi:10.1126/science.279.5349.362.
  34. ↑ Thomas-Keprta, K.L.; Clemett, S.J.; McKay, D.S.; Gibson, E.K.; Wentworth, S.J. (2009). "Origins of magnetite nanocrystals in Martian meteorite ALH84001". Geochimica et Cosmochimica Acta. 73 (21): 6631. Bibcode:2009GeCoA..73.6631T. doi:10.1016/j.gca.2009.05.064.
  35. ↑ Barber, D.J.; Scott, E.R.D. (2002). "Origin of supposedly biogenic magnetite in the Martian meteorite Allan Hills ALH84001". Proc. Natl. Acad. Sci. USA. 99: 6556. doi:10.1073/pnas.102045799.
  36. ↑ Agee, Carl B.; Wilson, Nicole V.; McCubbin, Francis M.; Ziegler, Karen; Polyak, Victor J.; Sharp, Zachary D.; Asmerom, Yemane; Nunn, Morgan H.; Shaheen, Robina (2013-02-15). "Unique Meteorite from Early Amazonian Mars: Water-Rich Basaltic Breccia Northwest Africa 7034". Science. 339 (6121): 780–785. ISSN 0036-8075. PMID 23287721. doi:10.1126/science.1228858.
  37. ↑ Ojha, Lujendra; Wilhelm, Mary Beth; Murchie, Scott L.; McEwen, Alfred S.; Wray, James J.; Hanley, Jennifer; Massé, Marion; Chojnacki, Matt (2015-11-01). "Spectral evidence for hydrated salts in recurring slope lineae on Mars". Nature Geoscience. 8 (11): 829–832. ISSN 1752-0894. doi:10.1038/ngeo2546.
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