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Gas-rich meteorites

Topic: Astronomy

 From HandWiki - Reading time: 15 min

Short description: Meteorites with high levels of primordial gases

Gas-rich meteorites are meteorites with high levels of primordial gases, such as helium, neon, argon, krypton, xenon and sometimes other elements.[1] Though these gases are present "in virtually all meteorites,"[2] the Fayetteville meteorite has ~2,000,000 x10−8 ccSTP/g helium,[3] or ~2% helium by volume equivalent. In comparison, background level is a few ppm.

The identification of gas-rich meteorites is based on the presence of light noble gases in large amounts, at levels which cannot be explained without involving an additional component over and above the well-known noble gas components that are present in all meteorites.[3]

History

William Ramsay was the first to report helium in an iron meteorite, in 1895- not long after its first Earth sample, instead of via Solar observation.[4]

The use of decay products to date meteorites was suggested by Bauer in 1947,[5] and explicitly published by Gerling and Pavlova in 1951.[6] However, this soon resulted in wildly varying ages; it was realized excess helium (including helium-3, rare on Earth) was generated by radiation, too.[7]

The first explicit publication of a gas-rich meteorite was Staroe Pesyanoe (often shortened to Pesyanoe), by Gerling and Levskii in 1956. In family with the later Fayetteville, Pesyanoe's helium level is ~1 million x10−8 ccSTP/g.[8]

Reynolds' publication of a "general Xe anomaly",[9] including 129I decay products and more, touched off the subfield of xenology,[10][11][12][13] continuing to today.[14][15]

The first publication of presolar grains in the 1980s[16] was precipitated by workers searching for noble gases;[17] PSGs were not simply checked via their gas contents.[18][19]

Lines of inquiry

As unreactive components, they are tracers of processes throughout and predating the Solar System:

Material age can be determined by relative exposure to direct solar and cosmic radiation (by cosmic ray tracks), and indirect creation of resultant nuclides. This includes Ar-Ar dating, I-Xe dating, and U to its various decay products including helium.[20][21][22]

The parent body of a meteorite can be traced in part via comparison of trace elements.[23][24][25] That meteorites are fragments of asteroids, and conditions on such asteroids, were partially deduced from gas evidence.[26][27][28][29]

This includes meteorite pairing, the re-association of meteorites which had split before recovery.[30][31]

Meteorite, parent, and Solar System histories are indicated by tracer elements,[32][33][34] including thermometry, a record of material temperature.[35]

The Lost City Meteor was tracked, allowing an orbit determination back to the asteroid belt. Measurement of relatively short-half-life isotopes in the subsequent Lost City Meteorite then indicate radiation levels in that region of the Solar System.[46]

Gas study

The field of meteoritic gases follows progress in analytical methods.[47]

The first analyses were basic laboratory chemistry, such as acid dissolution. Various acids were necessary, due to mixtures of various soluble and insoluble minerals. Stepped etching gave higher levels of resolution and discrimination.

Pyrolysis was used, such as on highly acid resistant minerals. These two methods were alternately lauded and derided as "burning the haystack to find the needle."[48][49][50]

Meteoritical studies have tracked the progress of mass spectrometry,[51] a continual and rapid progression[52][53] comparable to or greater than Moore's Law.[54]

More recently, laser extraction[55][56][57][58]

Meteorites

[59] This meteoritics-related list is incomplete; you can help by expanding it.

Name Classification Date Provenance Ref
Pantar H5 1938 Fall [60][61]
Fayetteville H4 1934 Fall [61][62][63]
Gladstone H4 1936 Find [64][65]
Noblesville H4 1991 Fall [66][67]
Tsukuba H5-6 1996 Fall [68][69]
Weston H4 1807 Fall [60][61][70]
Willard H3 1934 Find [71][65]
Elm Creek H4 1906 Find [61]
Leighton H5 1907 Fall [61][72]
Djermaia H 1961 Fall [61]
Acfer 111 -H3 1990 Find [73][74]
Ghubara L5 1954 Find [75][76]
St. Mesmin L5 1866 Fall [77][78][70]
(Staroe) Pesyanoe Aubrite 1933 Fall [79][63][80]
Khor Temiki Aubrite 1932 Fall [81][70]
Bustee Aubrite 1852 Fall [82][83]
Jodzie Howardite 1877 Fall [84]
Kapoeta Howardite 1942 Fall [85] 3[clarification needed],[86]
South Oman -EH 1958 Find [87][88]

Interplanetary dust, like c-chondrites and enstatites, contains hosts for these gases and often measurable gas contents.[89][90][91] So too do a fraction of micrometeorites.[92][56][93][94]

Gas

Gas components were first named by descriptors, then letter codes;[95][96] the letter taxonomy "has become increasingly complicated and confusing with time."[97][98]

By nuclide

Type Nuclides
Primordial/trapped 36Ar 132Xe[99]
Solar wind/solar flare 4He 20Ne 36Ar[96]
Cosmic ray/spallogenic 3He 83Kr 126Xe[7][100][101][102]
Radiogenic/fissile 3He 36Ar 40Ar 129Xe 132Xe 134Xe 136Xe 128Xe[103]

By component

A, Original Black 1972 letter code.[104] Soon found to be redundant.[105]

B, C, D

Original Black 1972 letter codes, attributed by him to the solar wind.[106][105]

E

Original Black 1972 letter code for "Exotic" neon- aberrant 20Ne/22Ne values.[107][108]

Planetary

"Planetary" gases (often shortened to "P") are depleted in light elements (He, Ne) compared to solar abundances (see below), or conversely, enriched in Kr, Xe.[109][110][111] This name originally implied an origin, the gas blend observed in terrestrial planets. Scientists wished to stop implying this,[112][111] but the habit was retained.[113][111]

P1, P2

Further developments of P, when all letters of the Latin alphabet were taken.[97]

Q, Q1, Q2

Different primordial gas blend, and its follow-on descriptors,[114][115] when all letters of the Latin alphabet were taken.[97]

Solar, subsolar

This gas component corresponds to the solar wind.[116][111] Solar flare gas can be distinguished by its greater depth,[117] and a slightly variant composition.[118] "Subsolar" is intermediary between solar and planetary.[119]

H

"Heavy" isotopes of xenon,[120][98] primarily r-process isotopes, plus p-process. Thus, sometimes seen as "HL," anomalous heavy and light isotopes.

G

"Giant", after asymptotic giant branch (while A and B had been taken[107][108]); contains their s-process isotopes.[121]

See also

References

  1. ↑ Suess, H. E.; Wänke, H.; Wlotzka, F. (1964-05-01). "On the origin of gas-rich meteorites". Geochimica et Cosmochimica Acta 28 (5): 595–607. doi:10.1016/0016-7037(64)90080-8. Bibcode: 1964GeCoA..28..595S. 
  2. ↑ Swindle, T. (1988). Trapped noble gases in meteorites. Tucson: University of Arizona Press. p. 535. Bibcode: 1988mess.book..535S.  in Meteorites and the early solar system, J. F. Kerridge & M. S. Matthews Eds.
  3. ↑ 3.0 3.1 Goswami, J.; Lal, D.; Wilkening, L. (1983). "Gas-Rich meteorites: Probes for particle environment and dynamical processes in the inner solar system". Space Science Reviews 37 (1–2): 111–59. doi:10.1007/BF00213959. Bibcode: 1984SSRv...37..111G. 
  4. ↑ Ramsay, W. (4 Jul 1895). "Argon and Helium in Meteoritic Iron". Nature 52 (1340): 224–25. doi:10.1038/052224a0. Bibcode: 1895Natur..52..224R. 
  5. ↑ Bauer, C. (15 August 1947). "Production of Helium in Meteorites by Cosmic Radiation". Physical Review 72 (4): 354. doi:10.1103/PhysRev.72.354. Bibcode: 1947PhRv...72..354B. 
  6. ↑ Gerling, E.; Pavlova, T. (1951). "Determination of the geological age of two stony meteorites by the argon method". Doklady Akademii Nauk SSSR 77: 85–97. 
  7. ↑ 7.0 7.1 Paneth, F.; Reasbeck, P.; Mayne, K. (Aug 1953). "Production by cosmic rays of helium-3 in meteorites". Nature 172 (4370): 200–01. doi:10.1038/172200a0. PMID 13087152. Bibcode: 1953Natur.172..200P. 
  8. ↑ Gerling, E.; Levskii, L. (1956). "On the origin of the rare gases in stony meteorites". Doklady Akademii Nauk SSSR 110: 750. 
  9. ↑ Reynolds, J. (15 May 1963). "Xenology". Journal of Geophysical Research 68 (10): 2939–56. doi:10.1029/JZ068i010p02939. Bibcode: 1963JGR....68.2939R. 
  10. ↑ Fleischer, R.; Price, P.; Walker, R. (1975). "6.5 Study of Nucleosynthesis and the Early History of the Solar System by Extinct Isotopes". Nuclear Tracks in Solids: Principles and Applications. University of California Press. ISBN 9780520026650. https://archive.org/details/bub_gb_yfTBvben3GoC. 
  11. ↑ Hintenberger, H. (Jul 1972). "Xenon in irdischer und in extraterrestrischer Materie (Xenologie)". Naturwissenschaften 59 (7): 285–91. doi:10.1007/BF00593352. Bibcode: 1972NW.....59..285H. 
  12. ↑ Kuroda, P. (Jan 1976). "Xenology: The enigma of xenon in carbonaceous chondrite". Geochemical Journal 10 (3): 121–36. doi:10.2343/geochemj.10.121. Bibcode: 1976GeocJ..10..121K. 
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  15. ↑ Diehl, R.; Hartmann, D.; Prantzos, N. (2018). "2.2.4 Extinct Radioactivity and Immediate Pre-Solar Nucleosynthesis". Astrophysics with Radioactive Isotopes (2nd ed.). Springer. ISBN 978-3319919294. 
  16. ↑ Lewis, R.; Ming, T.; Wacker, J.; Anders, E.; Steel, E. (Mar 1987). "Interstellar diamonds in meteorites". Nature 326 (6109): 160–62. doi:10.1038/326160a0. Bibcode: 1987Natur.326..160L. 
  17. ↑ Zinner, E.; Ming, T.; Anders, E. (24 Dec 1987). "Large isotopic anomalies of Si, C, N and noble gases in interstellar silicon carbide from the Murray meteorite". Nature 330 (6150): 730–32. doi:10.1038/330730a0. Bibcode: 1987Natur.330..730Z. 
  18. ↑ Ott, U. (Jul 1993). "Interstellar grains in meteorites". Nature 364 (6432): 25–33. doi:10.1038/364025a0. Bibcode: 1993Natur.364...25O. 
  19. ↑ 19.0 19.1 Anders, E. (1988). Circumstellar material in meteorites: noble gases, carbon and nitrogen. Tucson: University of Arizona Press. p. 927. ISBN 978-0816510634.  in Meteorites and the Early Solar System, Kerridge, J., Matthews, M. eds.
  20. ↑ Martin, G. (1953). "Recent studies of iron meteorites. IV The origin of meteoritic helium and the age of meteorites". Geochimica et Cosmochimica Acta 3 (6): 288–309. doi:10.1016/0016-7037(53)90037-4. Bibcode: 1953GeCoA...3..288M. 
  21. ↑ Gerling, E.; Pavlova, T. (1951). "Determination of the geological age of two stony meteorites by the argon method". Doklady Akademii Nauk SSSR 77: 85–97. 
  22. ↑ Wasserburg, G.; Hayden, R. (1955). "Age of meteorites by the Ar40-K40 method". Physical Review 97 (1): 86–87. doi:10.1103/PhysRev.97.86. Bibcode: 1955PhRv...97...86W. https://authors.library.caltech.edu/5266/1/WASpr55.pdf. 
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  30. ↑ Schultz, L.; Kruse, H.. "He, Ne, and Ar in meteorites. A detailed compilation". Meteoritics 24: 155–72. doi:10.1111/j.1945-5100.1989.tb00958.x. 
  31. ↑ Bogard, D; Johnson, P (Aug 1983). "Martian Gases in an Antarctic Meteorite?". Science 221 (4611): 651–54. doi:10.1126/science.221.4611.651. PMID 17787734. Bibcode: 1983Sci...221..651B. 
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  34. ↑ Begemann, F. (1972). "Ar37/Ar39 activity ratios in meteorites and the spatial consistency of the cosmic radiation". Journal of Geophysical Research 77: 3650–59. doi:10.1029/JB077i020p03650. Bibcode: 1972JGR....77.3650B. 
  35. ↑ Okazaki, R.; Nagao, K. (Apr 2017). "Primordial and cosmogenic noble gases in the Sutter's Mill CM chondrite". Meteoritics & Planetary Science 52 (4): 669–89. doi:10.1111/maps.12819. Bibcode: 2017M&PS...52..669O. 
  36. ↑ 36.0 36.1 Alaerts, L.; Lewis, R.; Matsuda, J; Anders, E. (1980). "Isotopic anomalies of noble gases in meteorites and their origins-Presolar components in the Murchison C2 chondrite". Geochimica et Cosmochimica Acta 44 (2): 189–209. doi:10.1016/0016-7037(80)90131-3. Bibcode: 1980GeCoA..44..189A. 
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  44. ↑ Wieler, R.; Pedroni, A.; Leya, I. (4 Feb 2010). "Cosmogenic neon in mineral separates from Kapoeta: No evidence for an irradiation of its parent body regolith by an early active Sun". Meteoritics & Planetary Science 35 (2): 251–57. doi:10.1111/j.1945-5100.2000.tb01774.x. 
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  46. ↑ Begemann, F. (10 Jul 1972). "Argon 37/argon 39 activity ratios in meteorites and the spatial constancy of the cosmic radiation". Journal of Geophysical Research 77 (20): 3650–59. doi:10.1029/JB077i020p03650. Bibcode: 1972JGR....77.3650B. 
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  50. ↑ Dauphas, N.; Schauble, E. (2016). "Mass Fractionation Laws, Mass-Independent Effects, and Isotopic Anomalies". Annu. Rev. Earth Planet. Sci. 44: 709–83. doi:10.1146/annurev-earth-060115-012157. Bibcode: 2016AREPS..44..709D. 
  51. ↑ Merrill, G. (Jun 1909). "The composition of stony meteorites compared with that of terrestrial igneous rocks, and considered with reference to their efficacy in world-making". American Journal of Science 27 (162): 469–74. doi:10.2475/ajs.s4-27.162.469. Bibcode: 1909AmJS...27..469M. https://zenodo.org/record/2101871. 
  52. ↑ Gilmour, J.; Lyon, I.; Johnston, W.; Turner, G. (Mar 1994). "RELAX: An ultrasensitive; resonance ionization mass spectrometer for xenon". Review of Scientific Instruments 65 (3): 617–25. doi:10.1063/1.1145127. Bibcode: 1994RScI...65..617G. 
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  54. ↑ Thompson, Bruce (15 Nov 2012). "Driving High Sensitivity in Biomolecular MS". Genetic Engineering & Biotechnology News 32 (20). 
  55. ↑ Takaoka, N.; Nagao, K.; Miura, Y. (1991). Noble Gas Study of Unique Meteorite Yamato-74063 by Laser Extraction. NIPR (Japan). p. 92.  in 16th Symposium on Antarctic Meteorites, Jun 5-7 1991
  56. ↑ 56.0 56.1 Stuart, F. M.; Harrop, P. J.; Knott, S.; Turner, G. (October 1999). "Laser extraction of helium isotopes from Antarctic micrometeorites: source of He and implications for the flux of extraterrestrial 3He to earth". Geochimica et Cosmochimica Acta 63 (17): 2653–2665. doi:10.1016/S0016-7037(99)00161-1. 
  57. ↑ Osawa, T.; Nagao, K.; Nakamura, T.; Takaoka, N. (2000). "Noble gas measurement in individual micrometeorites using laser gas-extraction system". Antarctic Meteorite Research 13: 322–41. Bibcode: 2000AMR....13..322O. 
  58. ↑ Avice, G.; Bekaert, D.; Chennaoui Aoudjehane, H.; Marty, B. (9 Feb 2018). "Noble gases and nitrogen in Tissint reveal the composition of the Mars atmosphere". Geochemical Perspectives Letters 6: 11–16. doi:10.7185/geochemlet.1802. 
  59. ↑ Padia, J.; Rao, M. (Jun 1989). "Neon isotope studies of Fayetteville and Kapoeta meteorites and clues to ancient solar activity". Geochimica et Cosmochimica Acta 53 (6): 1461–67. doi:10.1016/0016-7037(89)90078-1. Bibcode: 1989GeCoA..53.1461P. 
  60. ↑ 60.0 60.1 Eugster, O. (2003). "Cosmic-ray Exposure Ages of Meteorites and Lunar Rocks and Their Significance". Geochemistry 63 (1): 3–30. doi:10.1078/0009-2819-00021. Bibcode: 2003ChEG...63....3E. 
  61. ↑ 61.0 61.1 61.2 61.3 61.4 61.5 Graf, Thomas; Marti, Kurt (1995). "Collisional history of H chondrites". Journal of Geophysical Research 100 (E10): 21247. doi:10.1029/95JE01903. Bibcode: 1995JGR...10021247G. 
  62. ↑ Padia, J., Rao, M. "Neon isotope studies of Fayetteville and Kapoeta meteorites and clues to ancient solar activity ". (Jun 1989). Geochimica et Cosmochimica Acta. 53(6): 1461-67.
  63. ↑ 63.0 63.1 Mueller, O., Zahringer, J. "Chemische Unterschiede bei urdelgashaltigen Steinmeteoriten". (1966). Earth Planet. Sci. Lett. (1): 25.
  64. ↑ Miura, Y.; Nagao, K. (1992). "Noble gases and 81Kr-Kr exposure ages of non-Antarctic ordinary chondrites: An attempt to measure terrestrial ages of Antarctic meteorites". in Yanai, K.. Sixteenth Symposium on Antarctic Meteorites, held June 5–7, 1991, at the National Institute of Polar Research, Tokyo. National Institute of Polar Research (Japan). pp. 298–309. Bibcode: 1992AMR.....5..298M. https://core.ac.uk/download/pdf/51484034.pdf. Retrieved 2020-02-04. 
  65. ↑ 65.0 65.1 Osawa, T.; Nagao, K. (2006). "Noble gases in solar-gas-rich and solar-gas-free polymict breccias". Antarctic Meteorite Research 19: 58–78. Bibcode: 2006AMR....19...58T. 
  66. ↑ Lipschutz, M.; Wolf, S.; Vogt, S. (Sep 1993). "Consortium study of the unusual H chondrite regolith breccia, Noblesville". Meteoritics 28 (4): 528–537. doi:10.1111/j.1945-5100.1993.tb00276.x. Bibcode: 1993Metic..28..528L. 
  67. ↑ Murer, C.; Baur, H.; Signer, P.; Wieler, R. (Mar 1997). "Helium, neon, and argon abundances in the solar wind: In vacuo etching of meteoritic iron-nickel". Geochimica et Cosmochimica Acta 61 (6): 1303–14. doi:10.1016/S0016-7037(97)83772-6. Bibcode: 1997GeCoA..61.1303M. 
  68. ↑ Jabeen, I.; Kusakabe, M.; Nagao, K.; Nakamura, T. (1998). "Tsukuba meteorite: H chondrite, or a new parent body?". Meteoritics & Planetary Science 33: 77. 
  69. ↑ Nakashima, D.; Nakamura, T.; Sekiya, M.; Takaoka, N. (2002). "Cosmic-ray exposure age and heliocentric distance of the parent body of H chondrites Y75029 and Tsukuba". Antarctic Meteorite Research 15: 97–113. 
  70. ↑ 70.0 70.1 70.2 Schultz, L., Kruse, H. "Helium, Neon, and Argon in Meteorites: A Data Compilation". Max-Planck-Institut fur Chemie, Mainz. (1983).
  71. ↑ Inada, A.; Nagao, K. (2003). "Noble gases and cosmic-ray x host of Willard (b) H-chondrite: A breccia with". Meteoritics & Planetary Science 38: 5170. 
  72. ↑ Quijano-Rico, M.; Wanke, H. (1969). Millman, P. M.. ed. Meteorite Research: Proceedings of a Symposium on Meteorite Research Held in Vienna, Austria, 7–13 August 1968. Springer Science & Business Media. p. 134. ISBN 978-90-277-0132-9. 
  73. ↑ Romstedt, J.; Pedroni, A. (Jul 1993). "Irradiation History of ACFER 111, Inferred from Nuclear Tracks and Rare Gases". Meteoritics 28 (3): 424. Bibcode: 1993Metic..28R.424R. 
  74. ↑ Pedroni, A.; Begemann, F. (1994). "On unfractionated solar noble gas in the H3-6 meteorite Acfer 111". Meteoritics 29 (5): 632. doi:10.1111/j.1945-5100.1994.tb00776.x. 
  75. ↑ Levskii, L. (1979). "Rare gases in carbonaceous chondrites". Meteoritika 38: 27–36. Bibcode: 1979Metik..38...27L. 
  76. ↑ Meier, M.; Schmitz, B.; Alwmark, C. (2014). "He and Ne in individual chromite grains from the regolith breccia Ghubara (L5):Exploring the history of the L chondrite parent body regolith". Meteoritics & Planetary Science 49 (4): 576–94. doi:10.1111/maps.12275. Bibcode: 2014M&PS...49..576M. 
  77. ↑ Heymann, D.; Mazor, E. (1 Oct 1966). "St. Mesmin, A gas-rich amphoteric chondrite". Journal of Geophysical Research 71 (19): 4695–97. doi:10.1029/JZ071i019p04695. Bibcode: 1966JGR....71.4695H. 
  78. ↑ Schultz, L.; Signer, P. (Dec 1974). "Rare gasses in the St. Mesmin chondrite". Meteoritics 9: 402–03. Bibcode: 1974Metic...9..402S. 
  79. ↑ Gerling, E.; Levskii, L. (1956). "On the origin of the rare gases in stony meteorites". Doklady Akademii Nauk SSSR 110: 750. 
  80. ↑ Murty, S.; Marti, K. (Sep 1990). "Search for solar-type nitrogen in the gas-rich Pesyanoe meteorite". Meteoritics 25 (3): 227–30. doi:10.1111/j.1945-5100.1990.tb01000.x. Bibcode: 1990Metic..25..227M. 
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