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CM chondrite

Summary

CM chondrites are a group of chondritic meteorites which resemble their type specimen, the Mighei meteorite. The CM is the most commonly recovered group of the 'carbonaceous chondrite' class of meteorites, though all are rarer in collections than ordinary chondrites.

Overview and Taxonomy edit

Meteorites mostly divide into Ordinary and 'Carbonaceous' chondrite classes; far fewer belong to lesser classes like Enstatites and Ureilites. The term 'chondrite' indicates that these contain (or may have contained) chondrules in a matrix. Chondrules are cooled droplets of minerals, predating the meteorites themselves. The term 'carbonaceous' was assigned relative to the ordinary chondrites; some Enstatite and Ureilite meteorites may have more carbon than C-chondrites.[1] Still, all C-chondrites are distinguished from ordinary chondrites by a non-trace carbon content (resulting in a dark color), plus other volatiles, giving a lower density.[2][3] After the classes were devised, a more rigorous definition was found: C-chondrites contain proportionally higher magnesium than ordinary chondrites.[4][5][6]

The C-chondrites subdivide into CI, CM, CO, CV, CK, CR, and lesser groups (CH, CB, and ungrouped C-meteorites). Specimens are formed into groups by their petrological and chemical qualities, and the group named for a salient example. These include the CI (Ivuna-like), CM (Mighei-like), CO (Ornans-like), etc. The CM group most resembles the CI and CO chondrites; a CM-CO is sometimes described.[7][8][9] All three groups contain clearly anomalous 50Ti and 54Cr isotopes.[10][11]

Though the C-chondrites are far rarer than ordinary chondrites, the CM group is "the most abundant type of" them.[12][13] The latest Catalogue of Meteorites (5th edition, 2000) gives 15 CM falls (observed entries, then recoveries), and 146 finds (meteorites with entries unobserved, possibly ancient). By contrast, the next highest are the COs- 5 falls, 80 finds listed. These are in a class of 36 C-chondrite falls, 435 finds. If the CMs and COs are taken to be a clan, its dominance is even higher.[14]

Petrologic types edit

C-chondrites in general, and CM chondrites among them, have low densities for meteorites. CMs are slightly more dense (~2.1 gram/cc) than the CIs, but less dense than CO and other C-chondrites.[15][16] This is due to a combination of brecciation (rock lithified from fragments of prior rocks)[17] including porosities[2] and inherently light constituent materials (see chemistry, below). (Rare unbrecciated CMs include Y-791198 and ALH81002.[18])

Based primarily on petrology, early scientists attempted to quantify different meteorites. Rose ("kohlige meteorite"),[19] then Tschermak devised early taxonomies.[20] In the 1904 scheme of Brezina, today's CM chondrites would be "K" ("coaly chondrites").[21] Wiik published the first recognizably modern system in 1956, dividing meteorites into Type I, II, and III. CMs fell within Wiik's Type II.[22]

The CM chondrites are essentially all Type 2 in the petrographic scale of Van Schmus and Wood 1967; by that time, CI and CM recoveries were enough to define the 'left' (aqueous alteration) end of the scale. (CI chondrites, the Van Schmus Wood Type 1, is equivalent to Wiik's Type I, etc.) The types 4 through 6 indicate increasing thermal alteration; Type 3 is assumed to be unaltered.[23]

Type 1 2 3 4 5 6 7
Homogeneity of olivine and pyroxene compositions - >5% mean deviations ≤5% Homogeneous
Structural state of low-Ca pyroxene - Predominantly monoclinic >20% monoclinic ≤20% monoclinic Orthorhombic
Degree of development of secondary feldspar - Minor primary grains Secondary <2-um grains Secondary 2-50-um grains Secondary >50-um grains
Chondrule glass Altered or absent Mostly altered, some preserved Clear, isotropic Devitrified Absent
Metal: Maximum Ni content - <20% Taenite minor or absent >20% kamacite and taenite in exsolution relationship
Sulfides: Mean Ni content - >0.5% <0.5%
Overall Texture No chondrules Sharp chondrule boundaries Some chondrules can be discerned, fewer sharp edges Chondrules poorly delineated Primary textures destroyed
Matrix Fine-grained, opaque Mostly fine-grained opaque Opaque to transparent Transparent, recrystallized
Bulk carbon content ~2.8% ~0.6–2.8% ~0.2–1.0% <0.2%
Bulk water content ~20% ~4-18% 0.3-3% <1.5%

Van Schmus, Wood 1967; Sears, Dodd 1988; Brearley, Jones 1998; Weisberg 2006[8]

The modern groups 'V' and 'O' were named by Van Schmus in 1969 as divisions of Type 3, as 'subclass C3V' and 'C3O'.[24] Wasson then added C2M in 1974; since then, C2Ms have generally been shortened to simply 'CM', as have the other groups.[25]

Petrologic types by group
Group 1 2 3 4 5 6 7
CI
CM
CR
CH
CB
CV
CO
CK

After Weisberg et al. 2006,[8] Giese et al. 2019[26] Note: lone CV2 specimen, Mundrabilla 012[27][28]

Chondrules and similar edit

As Type 2 meteorites, CM chondrites have some remaining chondrules; others have been modified or dissolved by water. COs have more chondrules; CIs have either trace outlines of former chondrules ("pseudomorphs") or, some have argued, never contained any chondrules at all. Many CM chondrules are surrounded by either rims of accessory minerals, or haloes of water-altered chondrule material.[29][30]

The chondrules of CM chondrites, though fewer, are larger than in COs. While CM chondrules are smaller than average in diameter (~300 micrometer), CO chondrules are exceptionally small (~170 um).[31][32] This may be a survivor bias: consider that the water which dissolves CM chondrules successfully eliminates those which are already small, while those which were large may remain to be observed, though with less of the original material.[33] Similarly, CMs contain minor CAIs (calcium-aluminium rich inclusions).[34][35]

Matrix edit

The matrix of CMs (ground material, between chondrules) has been described as "sponge"[36] or "spongy."[24]

Grains of olivine and pyroxene silicates, too, are fewer in CM meteorites than COs, but more than CIs. As with chondrules, these are water-susceptible, and follow the water progression of the petrographic scale. So, too, do grains of free metal. CO meteorites contain higher levels of free metal domains, where CIs have mostly oxidized theirs; CMs are in between.[36][37]

Both free metal, and grains of olivine/pyroxene, have been largely or predominantly altered to matrix materials.[38] A CM meteorite will consist of more matrix than a CO, but less than a CI (which are essentially all matrix, per Van Schmus & Wood 1967).[39]

In 1860, Wohler presciently or coincidentally identified matrix as serpentinite.[40] Fuchs et al. 1973, unable to identify the constituent phyllosilicates, gave matrix as "poorly characterized phase" (PCP).[41] Cronstedtite was published by Kurat and Kracher in 1975.[42]

Tomeoka and Buseck, identifying cronstedtite and tochilinite in 1985, gave matrix material as “FESON” (Fe-Ni-S-O layers), as well as the backronym “partly characterized phase” for “PCP.”[43] Later authors would use the term TCI, tochilinite-cronstedtite intergrowths. Less common phyllosilicates include chlorite, vermiculite, and saponite.[44][45]

Sub-Classification edit

The CM group is both numerous and diverse. Multiple attempts have been made to subdivide the group beyond the Van Schmus-Wood typing. McSween 1979 was an early proposal.[46] After him, these add a suffix after the petrologic type, with 'CM2.9' referring to less-altered, CO-like specimens, and 'CM2.0' being more-altered, CI-like meteorites. (As of recently, no true 2.9 specimens have been catalogued.)

McSween 1979 graded the amount of matrix versus total amount, and the depletion of iron in the matrix, to quantify higher degrees of alteration.[46]

Browning et al. 1996 devised a formula ("MAI," Mineralogical Alteration Index), quantified the amount of unaltered silicate grains, and graded the alteration level of chondrules to quantify alteration.[47]

Rubin et al. 2007 added measurement of carbonates, with more dolomite and less calcite indicating higher alteration.[48]

Howard et al. 2009, 2011 measured total abundance of phyllosilicates to quantify alteration.[49][13]

Alexander et al. 2012, 2013 measured deuterium level, C/H, and nitrogen isotopes to quantify alteration.[50][51]

This line of inquiry continues, as the systems have some disagreement on specimens. Murchison is consistently ranked as low-alteration, but authors differ on some more-altered meteorites.

Transitional examples edit

CM-CO

  • Paris- described as "the least altered CM chondrite so far"[52] "that bridges the gap between CMs and COs"[53]
  • ALHA77307
  • Adelaide
  • Acfer 094
  • MAC87300, MAC88107

CM-CI

Water edit

The CI and CM chondrites are the "water rich" meteorites,[54][55][56] CMs having 3-14 wt% water.[57] Water is contained in tochilinite,[58][59] cronstedtite,[60] and others.[61][62][59]

This water, not comets,[63][64] was the likely origin of Earth's oceans via isotope tracing (primarily deuterium, but also others).[65][56]

Fluid inclusions edit

Fluid inclusions containing meteorite water have long been reported;[66][67][68] however, these claims were doubted due to, e. g., contamination by cutting fluids during sectioning.[69][70] More modern claims have taken steps such as waterless preparation.[71][72][73]

Chemistry edit

Carbonaceous chondrites, as the name suggests, contain appreciable carbon compounds.[74] These include native carbon, simple compounds like metal carbides and carbonates, organic chains, and polycyclic aromatic hydrocarbons (PAHs).[75][76]

The elemental abundances of some C-chondrite groups (with the obvious exception of hydrogen, helium, and some other elements, see below)[77][78] have long been known to resemble solar abundance values.[79][80][81] The CI chondrites, in particular, correspond "quite closely, more so than does any other type of meteoric or terrestrial matter";[82] called "somewhat miraculous".[8] Of course, only gas giant planets have the mass to retain, explicitly, hydrogen and helium. This extends to most noble gases, and to lesser amounts the elements N, O and C, the atmophiles. Other elements- volatiles and refractories- have correspondences between CI chondrites and the solar photosphere and solar wind such that the CI group is used as a cosmochemical standard.[83][84] As the Sun is 99% of the mass of the Solar System, knowing the solar abundance is the starting point for any other part or process of this System.[85]

The solar correspondence is similar but weaker in CM chondrites. More-volatile elements have been somewhat depleted relative to the CIs, and more-refractory elements somewhat enriched.[7][83][84]

A small amount[86] of meteorite materials are small presolar grains (PSGs).[87][88] These are crystals of material which survives from interstellar space, since before the formation of the Solar System. PSGs include silicon carbide ("Moissanite")[89] and micro-diamonds,[90] as well as other refractory minerals such as corundum and zircon.[91] The isotope levels of their elements do not match solar system levels, instead being closer to e. g., the interstellar medium. PSGs themselves may contain smaller PSGs.[92]

As with other meteorite classes, some carbon content is as carbides (often Cohenite, Fe3C with e.g., nickel substitutions)[93] and carbonates such as calcite and dolomite.[94][95][96] Aragonite appears, where CIs contain little or none.[97]

Total carbon compounds in CM chondrites are lower than in CI chondrites; however, more are aromatics.[98] Isotope profiling indicates these are meteoritic, not terrestrial.[99]

The organics of C-chondrites divide into soluble, and IOM (Insoluble Organic Matter). The soluble fraction would yield to the chemistry techniques of the mid-20th century,[100][101] giving paraffin, naphthene and aromatics, with other contributions.[102]

The IOM is, however, the clear majority of the organic component; in 1963, Briggs and Mamikunian could only give it as "very high molecular weight". IOM itself divides into two components: thermally labile, and refractory.[103]

Amino acids edit

Amino acids and other organics were first reported by multiple groups;[104][105] however, concentrations were low to undetectable,[106][107] and claimed to be terrestrial contamination.[108][109] The 1969 fall of the Murchison meteorite provided over 100 kg of sample, the largest CM ever. Specimens were recovered quickly, from a dry area. Combined with progress in, e.g., biochemistry and petrochemistry techniques, the question could be addressed more definitively: sugars[110] and amino acids[111][112] existed in space, via meteorites. This includes non-terrestrial amino acids.[113][114] Multiple isotopes do not match Earth levels, strong evidence for non-contamination.[115][116][117]

The levels of amino acids are higher in CMs than CIs.[118]

Amino-like nitriles/cyanides[119] and heterocycles[120] are also found. These related organics may be decomposition products or precursors.[121][122][123]

Chirality edit

The early analyses did not record optical rotation, and gave meteoritic organics as racemic.[124][102] As amino acids are diverse but low, the discovery of meteoritic chirality had to await the separation of IOM.[125] Handedness of some meteorite organics is now accepted (see below),[116] including in the soluble organic fraction.[126][127]

Meteoritic Amino Acids
Amino Acid Ref
Glycine 1
Alanine 1
Serine 5
Isoserine 4
Homoserine 4
β-Homoserine 4
d-2,3-diaminopropanoic acid 2
α-Methylserine 4
Threonine 5
Isothreonine 4
allo-Isothreonine 4
Asparagine 5
2,3-Diaminobutanoic acid 2
Glutamic acid 1
Valine 1
Isovaline 3
Norvaline 3
Proline 1
Leucine 5
Isoleucine 5
Norleucine 3
2-methylalanine 1
Isobutylamine 6
Histamine 5
Isovaline 6
Sarcosine 1

1. Kvenvolden et al. 1970;[113] 2. Meierheinrich[128] et al. 2004 3. Martins et al. 2015[129] 4. Koga et al. 2017;[114] 5. Rudraswami et al. 2018;[130] 6. Pizzarello, Yarnes 2018[127]

Gas edit

The first publication of anomalous gas in a carbonaceous chondrite (Murray) was in 1960.[131] "Gas-rich meteorites" of other classes host their gas in dark liths,[132] in most cases closely related to CM.[133]

Gases in meteorites include primordial, solar (both solar wind, and a distinct solar flare component), radiogenic (due to cosmic-ray exposure), and fissile (decay products).[134] Host materials are generally carbonaceous,[135] including presolar grains: diamond,[136] silicon carbide,[137][138] graphite,[139] and organics.

Nogoya is one particularly gas-rich CM chondrite.[132][140]

Micrometeorites lose significant amounts of their gas to entry heating,[141] but still deliver quantifiable amounts.[142]

Isotopic analyses edit

Isotope studies have become vital in examining natural histories.[143] Oxygen, in particular, forms quite stable oxides; it requires significant events, processes, or energies to segregate isotopes by their slight mass differences.

CM and CI chondrites have a measurable difference in oxygen isotope levels. This suggests a different formation temperature, and hence a different zone of the young Solar System. However, CM and CO meteorites were found to have similar oxygen isotopes, indicating a relationship.[7][144][145]

Hydrogen edit

Carbon edit

Nitrogen edit

Provenance edit

CMs, like other C-chondrites, are subjected to a serious observation bias. C-chondrites are friable, due to both macro-scale porosity and micro-scale matrices of phyllosilicates, with many chondrules also having layers such as phyllosilicates.[146] The meteorites have been described as "tuff" (compacted volcanic ash).[147][29]

As one example, the Tagish Lake meteorite provided ~10 kg of samples, from a meteor estimated to be 60-90 tons before entry.[148]

By contrast, many ordinary chondrite meteorites are tougher[149] and overrepresented.[150] Iron meteorites are even moreso.[151]

CI and CM chondrites in particular are then subject to weathering on the ground. As large fractions of C-chondrite material are water soluble, ordinary chondrites and irons are more likely to be recognized and recovered. Greater coverage of hot deserts and Antarctica has resulted in many C-chondrite specimens.[152][153][154]

Parent body(s) edit

As carbonaceous specimens, CM and other groups are widely assumed to be from carbonaceous asteroids. This includes the explicit C-type asteroids, and to various degrees the related G-, B- (including the deprecated F-), D-, and P-types.[155][156][157] As carbonaceous types are the majority of asteroids,[158][159][160] but only a few percent of recovered meteorites,[14] selection/filtering effects must be severe.

Aside from the diversity of CMs, and the diversity of C-asteroid types and subtypes (besides the asteroids themselves), the question of parentage is very open as of this writing. The Almahata Sitta meteorite was catalogued as a ureilite, an entirely different meteorite class. However, it entered as asteroid 2008 TC3. A crude spectrum was taken before entry, which would have placed 2008 TC3 as a F- or B-type.[161]

Some amount of space weathering is seen to occur on carbonaceous asteroids; this complicates attempts to link parents via spectroscopy.[162][163][164]

A hypothesis persists that all CMs stem from a single parent.[7][165][166]

An alternate hypothesis[167][168]

Polymict meteorites edit

Brecciated meteorites include monomict breccias (re-formed from rock fragments on a single type) and polymict ones (incorporating different source rocks). Polymict meteorites record exchanges between sites. C-chondrite materials are often found in such meteorites.[169][170]

  • PRA 04401- nominally a HED, contains as much CM or CM-like material in clasts as HED material[171]
  • Kaidun- a "kitchen sink"[172] breccia
  • Supuhee
  • Plainview
  • Jodzie

Micrometeorites/Interplanetary Dust Particles (IDPs) edit

Open issues edit

List of CM chondrites edit

Notable specimens edit

  • Mighei- 1889; from which the group name derives
  • Cold Bokkevelt- 1838; a find, but from an arid region, and considered reasonably unaltered
  • Nogoya- 1879;
  • Boriskino- 1930;
  • Murray- 1950;
  • Murchison- 1969; large total known weight of 100 kg recovered, resulting in extensive study
  • Yamato 74662- 1974; first Antarctic CM

Recently recovered CM chondrites edit

  • Aguas Zarcas- Apr 2019 fall, specimens recovered quickly; >20 kg
  • Winchcombe meteorite
  • Mukundpura meteorite- 6 June 2017 fall, broke up during impact; 2.2 kg of fragments were recovered within hours

See also edit

General References edit

  • Mason, B. The Carbonaceous Chondrites. 1962 Space Sciences Reviews vol. 1, p. 621
  • Meteorites and the Early Solar System, Kerridge, J. Matthews, M. eds. 1988 University of Arizona Press, Tucson ISBN 9780816510634
  • Planetary Materials, Papike, J., ed. 1999 Mineralogical Society of America, Washington DC ISBN 0-939950-46-4
  • The Catalogue of Meteorites, Grady, M. ed. 2000 Cambridge University Press, Cambridge ISBN 0 521 66303 2
  • Meteorites and the Early Solar System II, Lauretta, D. McSween, H. eds. 2006 University of Arizona Press, Tucson ISBN 9780816525621

References edit

  1. ^ Scott, E; Krot, A (2003). Treatise on Geochemistry. Vol. 1. Elsevier. p. 143. ISBN 0-08-043751-6. Ch. Chondrites and their Components
  2. ^ a b Britt, D (Jul 2000). "The porosity of dark meteorites and the structure of low-albedo asteroids". Icarus. 143 (1): 213. Bibcode:2000Icar..146..213B. doi:10.1006/icar.2000.6374.
  3. ^ Macke, R; Consolmagno, G; Britt, D (Nov 2011). "Density, porosity, and magnetic susceptibility of carbonaceous chondrites". Meteoritics & Planetary Science. 46 (12): 1842. Bibcode:2011M&PS...46.1842M. doi:10.1111/j.1945-5100.2011.01298.x. S2CID 128721593.
  4. ^ Urey, H (Jun 1961). "Criticism of Dr. B. Mason's paper on "The origin of meteorites"". Journal of Geophysical Research. 66 (6): 1988. Bibcode:1961JGR....66.1988U. doi:10.1029/JZ066i006p01988.
  5. ^ Ahrens, L (1964). "Si-Mg fractionation in chondrites". Geochimica et Cosmochimica Acta. 28 (4): 411. Bibcode:1964GeCoA..28..411A. doi:10.1016/0016-7037(64)90115-2.
  6. ^ Ahrens, L (1965). "Observations on the Fe-Si-Mg relationship in chondrites". Geochimica et Cosmochimica Acta. 29 (7): 801. Bibcode:1965GeCoA..29..801A. doi:10.1016/0016-7037(65)90032-3.
  7. ^ a b c d Kallemeyn, G; Wasson, J (1981). "The compositional classification of chondrites-I. The carbonaceous chondrite groups". Geochimica et Cosmochimica Acta. 45 (7): 1217. Bibcode:1981GeCoA..45.1217K. doi:10.1016/0016-7037(81)90145-9.
  8. ^ a b c d Weisberg, M; McCoy, T; Krot, A (2006). "Systematics and Evaluation of Meteorite Classification". Meteorites and the Early Solar System II. Vol. 45. Tucson: University of Arizona Press. p. 19. Bibcode:1981GeCoA..45.1217K. doi:10.1016/0016-7037(81)90145-9. {{cite book}}: |journal= ignored (help)
  9. ^ "CM-CO clan chondrites". Meteoritical Bulletin: Search the Database. The Meteoritical Society. Retrieved 10 Sep 2019.
  10. ^ Trinquier, A; Elliott, T; Ulfbeck, D; Coath, C; Krot, A; Bizzarro, M (17 Apr 2009). "Origin of Nucleosynthetic Isotope Heterogeneity in the Solar Protoplanetary Disk". Science. 324 (5925): 374–6. Bibcode:2009Sci...324..374T. doi:10.1126/science.1168221. PMID 19372428. S2CID 6120153.
  11. ^ Qin, L; Rumble, D; Alexander, C; Carlson, R; Jenniskens, P; Shaddad, M (2010). "The chromium isotopic composition of Almahata Sitta". Meteoritics & Planetary Science. 45 (1533): 1771. Bibcode:2010LPI....41.1910Q. doi:10.1111/j.1945-5100.2010.01109.x. S2CID 55170869.
  12. ^ McSween, H (1979). "Alteration in CM carbonaceous chondrites inferred from modal and chemical variations in matrix". Geochimica et Cosmochimica Acta. 43 (11): 1761. Bibcode:1979GeCoA..43.1761M. doi:10.1016/0016-7037(79)90024-3.
  13. ^ a b Howard, K; Benedix, G; Bland, P; Cressey, G (2011). "Modal mineralogy of CM chondrites by X-ray Diffraction (PSR-XRD)". Geochimica et Cosmochimica Acta. 75: 2735. doi:10.1111/j.1945-5100.2004.tb00046.x.
  14. ^ a b Grady, M (2000). The Catalogue of Meteorites. Cambridge: Cambridge University Press. ISBN 0-521-66303-2.
  15. ^ Britt, D; Consolmagno, G (August 2003). "Stony meteorite porosities and densities: A review of the data through 2001". Meteoritics & Planetary Science. 38 (8): 1161. Bibcode:2003M&PS...38.1161B. doi:10.1111/j.1945-5100.2003.tb00305.x. S2CID 55612044.
  16. ^ Carry, B (2012). "Density of asteroids". Planetary and Space Science. 73 (1): 98. arXiv:1203.4336. Bibcode:2012P&SS...73...98C. doi:10.1016/j.pss.2012.03.009. S2CID 119226456.
  17. ^ Bischoff, A; Ebert, S; Metzler, K; Lentfort, S (2017). Breccia Classification of CM Chondrites. 80th Meteoritical Society. Bibcode:2017LPICo1987.6089B.
  18. ^ Chizmadia, L; Brearley, A (2004). Aqueous Alteration Of Carbonaceous Chondrites: New Insights From Comparative Studies Of Two Unbrecciated CM2 Chondrite, Y-791198 And ALH81002. LPS XXXV. Bibcode:2004LPI....35.1753C.
  19. ^ Rose, G (1863). Physik. Abhandl. Akad. Wiss. Berlin. p. 23.{{cite book}}: CS1 maint: location missing publisher (link)
  20. ^ Tschermak, G (1883). "Beitrag zur Classification der Meteoriten". Math. -Naturw. Cl. 85 (1). Sitzber. Akad. Wiss.: 347–71.
  21. ^ Brezina, A (1904). "The Arrangement of Collections of Meteorites". Proc. Am. Philos. Soc. 43 (176): 211–247. JSTOR 983506.
  22. ^ Wiik, H (1956). "The chemical composition of some stony meteorites". Geochimica et Cosmochimica Acta. 9 (5): 279. Bibcode:1956GeCoA...9..279W. doi:10.1016/0016-7037(56)90028-X.
  23. ^ Van Schmus, W; Wood, J (1967). "A chemical-petrologic classification for the chondritic meteorites". Geochimica et Cosmochimica Acta. 31 (5): 747. Bibcode:1967GeCoA..31..747V. doi:10.1016/S0016-7037(67)80030-9.
  24. ^ a b Millman, P., ed. (1969). "Mineralogical, Petrology, and Classification of Types 3 and 4 Carbonaceous Chondrites". Meteorite Research. Dordrecht: D. Reidel Publishing Company. p. 480. ISBN 978-94-010-3413-5.
  25. ^ Wasson, J (1974). Meteorites: Classification and Properties. New York: Springer-Verlag. ISBN 978-3-642-65865-5.
  26. ^ Giese, C Ten Kate I Plumper O King H Lenting C Liu Y Tielens A (Jul 2019). "The evolution of polycyclic aromatic hydrocarbons under simulated inner asteroid conditions". Meteoritics & Planetary Science. 54 (9): 1930. Bibcode:2019M&PS...54.1930G. doi:10.1111/maps.13359. hdl:1887/84978.
  27. ^ "Meteoritical Bulletin: Entry for Mundrabilla 012". Meteoritical Bulletin. The Meteoritical Society. Retrieved 14 Sep 2019.
  28. ^ "Mundrabilla 012 meteorite, Mundrabilla Roadhouse, Dundas Shire, Western Australia, Australia". Mindat.org. Retrieved 14 Sep 2019.
  29. ^ a b Bunch, T; Chang, S (1978). Carbonaceous chondrite (CM) phyllosilicates: condensation or alteration origin?. Lunar and Planetary Science IX. p. 134. Bibcode:1978LPI.....9..134B.
  30. ^ Metzler, K; Bischoff, A (Jan 1994). "Constraints on chondrule agglomeration from fine-grained chondrule rims". Chondrules and the Protoplanetary Disk, NASA-CR-197121. p. 23.
  31. ^ Rubin, A (Sep 1989). "Size‐frequency distributions of chondrules in CO3 chondrites". Meteoritics. 24 (3): 179. Bibcode:1989Metic..24..179R. doi:10.1111/j.1945-5100.1989.tb00960.x.
  32. ^ Choe, W; Huber, H; Rubin, A; Kallemeyn, G; Wasson, J (Apr 2010). "Compositions and taxonomy of 15 unusual carbonaceous chondrites". Meteoritics & Planetary Science. 45 (4): 531. Bibcode:2010M&PS...45..531C. doi:10.1111/j.1945-5100.2010.01039.x. S2CID 16839084.
  33. ^ Rubin, A (May 1998). "Correlated petrologic and geochemical characteristics of CO3 chondrites". Meteoritics & Planetary Science. 33 (2): 385. Bibcode:1998M&PS...33..385R. doi:10.1111/j.1945-5100.1998.tb01644.x. S2CID 129404145.
  34. ^ Rubin, A (Oct 2007). "Petrography of refractory inclusions in CM2.6 QUE 97990 and the origin of melilite‐free spinel inclusions in CM chondrites". Meteoritics & Planetary Science. 42 (10): 1711. Bibcode:2007M&PS...42.1711R. doi:10.1111/j.1945-5100.2007.tb00532.x.
  35. ^ Hezel, D; Russell, S; Ross, A; Kearsley, A (2008). "Modal abundances of CAIs: Implications for bulk chondrite element abundances and fractionations". Meteoritics & Planetary Science. 43 (11): 1879. arXiv:0810.2174. Bibcode:2008M&PS...43.1879H. doi:10.1111/j.1945-5100.2008.tb00649.x. S2CID 119289798.
  36. ^ a b Barber, D (1977). "The Matrix of C2 and C3 Carbonaceous Chondrites". Meteoritics. 12: 172. Bibcode:1977Metic..12..172B.
  37. ^ Barber, D (1981). "Matrix phyllosilicates and associated minerals in C2M carbonaceous chondrites". Geochimica et Cosmochimica Acta. 45 (6): 945. Bibcode:1981GeCoA..45..945B. doi:10.1016/0016-7037(81)90120-4.
  38. ^ Wood, J (1967). "Chondrites: Their metallic minerals, thermal histories, and parent planets". Icarus. 6 (1): 1–49. Bibcode:1967Icar....6....1W. doi:10.1016/0019-1035(67)90002-4.
  39. ^ Wood, J (Oct 1967). "Olivine and pyroxene compositions in type II carbonaceous chondrites". Geochimica et Cosmochimica Acta. 31 (10): 2095. Bibcode:1967GeCoA..31.2095W. doi:10.1016/0016-7037(67)90144-5.
  40. ^ Wöhler, F (1860). Sitzungsber. Akad. Wissensch. 41: 565. {{cite journal}}: Missing or empty |title= (help)
  41. ^ Fuchs, L; Olsen, E; Jensen, K (1973). "Mineralogy, mineral-chemistry, and composition of the Murchison (C2) meteorite". Smithsonian Contributions to the Earth Sciences (10): 1–39. doi:10.5479/si.00810274.10.1.
  42. ^ Kurat, G; Kracher, A (Dec 1975). "Preliminary report on the Cochabamba carbonaceous chondrite". Meteoritics. 10: 432–433. Bibcode:1975Metic..10..432K.
  43. ^ Tomeoka, K; Buseck, P (1985). "Indicators of aqueous alteration in CM carbonaceous chondrites". Geochimica et Cosmochimica Acta. 49 (10): 2149–2163. doi:10.1016/0016-7037(85)90073-0.
  44. ^ Barber, D (Dec 1985). "Phyllosilicates and other layer-structured minerals in stony meteorites". Clay Minerals. 20 (4): 415–454. doi:10.1180/claymin.1985.020.4.01. S2CID 129110766.
  45. ^ Lauretta, D; McSween, H (2006). "The Action of Water". Meteorites And The Early Solar System II. Tucson: University of Arizona Press. p. 588. ISBN 9780816525621.
  46. ^ a b McSween, H (1979). "Alteration in CM carbonaceous chondrites inferred from modal and chemical variations in matrix". Geochimica et Cosmochimica Acta. 43 (11): 1761. Bibcode:1979GeCoA..43.1761M. doi:10.1016/0016-7037(79)90024-3.
  47. ^ Browning, L; McSween, H; Zolensky, M (1996). "Correlated alteration effects in CM carbonaceous chondrites". Geochimica et Cosmochimica Acta. 60 (14): 2621. Bibcode:1996GeCoA..60.2621B. doi:10.1016/0016-7037(96)00121-4.
  48. ^ Rubin, A; Trigo-Rodriguez, J; Huber, H; Wasson, J (2007). "Progressive aqueous alterations of CM carbonaceous chondrites". Geochimica et Cosmochimica Acta. 71 (9): 2361. Bibcode:2007GeCoA..71.2361R. doi:10.1016/j.gca.2007.02.008.
  49. ^ Howard, K; Benedix, G; Bland, P; Cressey, G (Aug 2009). "Modal mineralogy of CM2 chondrites by X-ray diffraction (PSD-XRD). Part 1: Total phyllosilicate abundance and the degree of aqueous alteration". Geochimica et Cosmochimica Acta. 73 (15): 4576. Bibcode:2009GeCoA..73.4576H. doi:10.1016/j.gca.2009.04.038.
  50. ^ Alexander, C; Bowden, R; Fogel, M; Howard, K; Greenwood, R (Mar 2012). The Classification of CM and CR Chondrites Using Bulk H Abundances and Isotopes. 43rd LPSC.
  51. ^ Alexander, C; Howard, K; Bowden, R; Fogel, M (2013). "The classification of CM and CR chondrites using bulk H, C N abundances and isotopic compositions". Geochimica et Cosmochimica Acta. 123: 244. Bibcode:2013GeCoA.123..244A. doi:10.1016/j.gca.2013.05.019.
  52. ^ Hewins, R; Bourot-Denise, M; et al. (Jan 2014). "The Paris meteorite, the least altered CM chondrite so far". Geochimica et Cosmochimica Acta. 124: 190. Bibcode:2014GeCoA.124..190H. doi:10.1016/j.gca.2013.09.014.
  53. ^ Bourot-Denism, M; Zanda, B; Marrocchi, Y; Greenwood, R; Pont, S (Mar 2010). "Paris: The slightly altered, slightly metamorphosed CM that bridges the gap between CMs and COs". 41st LPSC (1683): 1683. Bibcode:2010LPI....41.1683B.
  54. ^ Ostrowski, D; Lacy, C; Gietzen, K; Sears, D (Feb 2011). "IRTF spectra for 17 asteroids from the C and X complexes: A discussionof continuum slopes and their relationships to C chondrites and phyllosilicates". Icarus. 212 (2): 682–696. Bibcode:2011Icar..212..682O. doi:10.1016/j.icarus.2011.01.032.
  55. ^ Alexander, C; McKeegan, K; Altwegg, K (Feb 2018). "Water Reservoirs in Small Planetary Bodies: Meteorites, Asteroids, and Comets". Space Science Reviews. 214 (1): 36. Bibcode:2018SSRv..214...36A. doi:10.1007/s11214-018-0474-9. PMC 6398961. PMID 30842688.
  56. ^ a b Trigo-Rodríguez, J; Rimola, A; Tanbakouei, S; Cabedo Soto, V; Lee, M (Feb 2019). "Accretion of water in carbonaceous chondrites: current evidence and implications for the delivery of water to early earth". Space Science Reviews. 215 (1): 18. arXiv:1902.00367. Bibcode:2019SSRv..215...18T. doi:10.1007/s11214-019-0583-0. S2CID 119196857.
  57. ^ D’Angelo, M; Cazaux, S; Kamp, I; Thi, W; Woitke, P (Feb 2019). "On water delivery in the inner solar nebula: Monte Carlo simulations of forsterite hydration". Astronomy & Astrophysics. 622: A208. arXiv:1808.06183. Bibcode:2019A&A...622A.208D. doi:10.1051/0004-6361/201833715. S2CID 55659350.
  58. ^ Gooding, J; Zolensky, M (Mar 1987). Thermal Stability Of Tochilinite. LPSC XVIII.
  59. ^ a b Nakamura, T; Matsuoka, M; Yamashita, S; Sato, Y; Mogi, K; Enokido, Y; Nakata, A; Okumura, S; Furukawa, Y; Zolensky, M (Mar 2017). Mineralogical, Spectral, and Compositional Changes During Heating of Hydrous Carbonaceous Chondrites. Lunar and Planetary Science XLVIII.
  60. ^ Beck, P; Quirico, E; Montes-Hernandez, G; Bonal, L; Bollard, J; Orthous-Daunay, F; Howard, K; Schmitt, B; Brissaud, O; Deschamps, F; Wunder, B; Guillot, S (2010). "Hydrous mineralogy of CM and CI chondrites from infrared spectroscopy and their relationship with low albedo asteroids". Geochimica et Cosmochimica Acta. 74 (16): 4881–4892. Bibcode:2010GeCoA..74.4881B. doi:10.1016/j.gca.2010.05.020.
  61. ^ Buseck, P; Hua, X (1993). "Matrices Of Carbonaceous Chondrite Meteorites". Annu. Rev. Earth Planet. Sci. 21: 255–305. Bibcode:1993AREPS..21..255B. doi:10.1146/annurev.ea.21.050193.001351.
  62. ^ Takir, D; Emery, J; Mcsween, H; Hibbitts, C; Clark, R; Pearson, N; Wang, A (Sep 2013). "Nature and degree of aqueous alteration in CM and CI carbonaceous chondrites". Meteoritics & Planetary Science. 48 (9): 1618–1637. Bibcode:2013M&PS...48.1618T. doi:10.1111/maps.12171. S2CID 129003587.
  63. ^ Morbidelli, A.; Chambers, J; Lunine, Jonathan I.; Petit, Jean-Marc; Robert, F.; Valsecchi, G.; Cyr, K. (2000). "Source regions and timescales for the delivery of water to the Earth". Meteoritics & Planetary Science. 35 (6): 1309–20. Bibcode:2000M&PS...35.1309M. doi:10.1111/j.1945-5100.2000.tb01518.x.
  64. ^ Hallis, L (28 May 2017). "D/H ratios of the inner Solar System". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 375 (2094): 20150390. Bibcode:2017RSPTA.37550390H. doi:10.1098/rsta.2015.0390. PMC 5394254. PMID 28416726.
  65. ^ Alexander, C; Bowden, R; Fogel, M; Howard, K; Herd, C; Nittler, L (10 Aug 2012). "The Provenances of Asteroids, and Their Contributions to the Volatile Inventories of the Terrestrial Planets". Science. 337 (6095): 721–723. Bibcode:2012Sci...337..721A. doi:10.1126/science.1223474. PMID 22798405. S2CID 206542013.
  66. ^ Yasinskaya, A (1969). "Inclusions in stony meteorites". In Roedder, E (ed.). Fluid Inclusion Research- Proc. COFFI 2. pp. 149–153.
  67. ^ Fieni, C; Bourot-Denise, M; Pellas, P; Touret, J (1978). "Aqueous fluid inclusions in feldspars and phosphates from Peetz Chondrite". Meteoritics. 13: 460–461. Bibcode:1978Metic..13..460F.
  68. ^ Mattey, D; Pillinger, C; Fallick, A (1983). "H isotopic composition of water in fluid inclusions in the Peetz L6 Chondrite". Meteoritics & Planetary Science. 18: 348.
  69. ^ Rudnick, R; Ashwal, L; Henry, D; Gibson, E (Mar 1984). "Fluid inclusions in stony meteorites—A cautionary note". Journal of Geophysical Research: Solid Earth. 90 Suppl (669): C669-75. doi:10.1029/jb090is02p0c669. PMID 11542002.
  70. ^ Bodnar, R; Zolensky, M (2000). "Title: Fluid Inclusions in Meteorites: Are They Useful, and Why are They So Hard to Find?". Meteoritics & Planetary Science. 35 (5): A29.
  71. ^ Saylor, J; Zolensky, M; Bodnar, R; Le, L; Schwandt, C (Mar 2001). "Fluid Inclusions In Carbonaceous Chondrites". LPS Xxxii (1875): 1875. Bibcode:2001LPI....32.1875S.
  72. ^ Zolensky, M (2010). "Liquid Water in Asteroids: Evidence from Fluid Inclusions in Meteorites". Astrobiology Science Conference 2010. 1538 (5278): 5278. Bibcode:2010LPICo1538.5278Z.
  73. ^ Yurimoto, H; Itoh, S; Zolensky, M (Oct 2014). "Isotopic compositions of asteroidal liquid water trapped in fluid inclusionsof chondrites". Geochemical Journal. 48 (6): 549–560. Bibcode:2014GeocJ..48..549Y. doi:10.2343/geochemj.2.0335. hdl:2115/57641.
  74. ^ Pearson, V; Sephton, M; Franchi, I; Gibson, J; Gilmour, I (Jan 2010). "Carbon and nitrogen in carbonaceous chondrites: Elemental abundances and stable isotopic compositions". Meteoritics & Planetary Science. 41 (12): 1899. Bibcode:2006M&PS...41.1899P. doi:10.1111/j.1945-5100.2006.tb00459.x. S2CID 59383820.
  75. ^ Hayes, J (Sep 1967). "Organic constituents of meteorites—a review". Geochimica et Cosmochimica Acta. 31 (9): 1395–1440. doi:10.1016/0016-7037(67)90019-1.
  76. ^ Botta, O; Bada, J (Jan 2002). "Extraterrestrial Organic Compounds in Meteorites". Surveys in Geophysics. 23 (5): 411–67. Bibcode:2002SGeo...23..411B. doi:10.1023/A:1020139302770. S2CID 93938395.
  77. ^ Holweger, H (Feb 1977). "The solar Na/Ca and S/Ca ratios: A close comparison with carbonaceous chondrites". Earth and Planetary Science Letters. 34 (1): 152. Bibcode:1977E&PSL..34..152H. doi:10.1016/0012-821X(77)90116-9.
  78. ^ Anders, E; Ebihara, M (Nov 1982). "Solar-system abundances of the elements". Geochimica et Cosmochimica Acta. 46 (11): 2363. Bibcode:2014pacs.book...15P. doi:10.1016/0016-7037(82)90208-3.
  79. ^ Suess, H (1949). "Die kosmische häufigkeit der chemischen elemente". Experientia. 5 (7): 266–70. doi:10.1007/BF02149939. PMID 18146573. S2CID 11969464.
  80. ^ Suess, H Urey H (Jan 1956). "Abundances of the Elements". Rev. Mod. Phys. 28 (1): 53. Bibcode:1956RvMP...28...53S. doi:10.1103/RevModPhys.28.53.
  81. ^ Asplund, M; Grevesse, N; Sauval, AJ; Scott, P (2009). "The chemical composition of the Sun". Annual Review of Astronomy & Astrophysics. 47 (1): 481–522. arXiv:0909.0948. Bibcode:2009ARA&A..47..481A. doi:10.1146/annurev.astro.46.060407.145222. S2CID 17921922.
  82. ^ Anders, E (Dec 1964). "Origin, age, and composition of meteorites". Space Science Reviews. 3 (5–6): 5. Bibcode:1964SSRv....3..583A. doi:10.1007/BF00177954. S2CID 122077103.
  83. ^ a b Goswami, A; Eswar Reddy, B, eds. (2010). "Solar system abundances of the elements". Principles and Perspectives in Cosmochemistry: Lecture Notes of the Kodai School on 'Synthesis of Elements in Stars' held at Kodaikanal Observatory, India, April 29 - May 13, 2008. Heidelberg: Springer-Verlag. p. 379. ISBN 978-3-642-10351-3.
  84. ^ a b Davis, A (2014). "Solar System Abundances of the Elements". Planets, Asteroids, Comets and The Solar System, Treatise on Geochemistry, Vol. 2 (2nd ed.). Elsevier. p. 21. ISBN 978-0080999432.
  85. ^ Russell, C (Jan 2003). "Foreword". Space Science Reviews. 105 (3): vii. Special Issue: The Genesis Discovery Mission
  86. ^ Leitner, J; Hoppe, P; Metzler, K; Haenecour, P; Floss, C; Vollmer, C (2015). The Presolar Grain Inventory Of CM Chondrites. 78th Meteoritical Society Meeting. Bibcode:2015LPICo1856.5178L.
  87. ^ Huss, G; Meshik, A; Smith, J; Hohenberg, C (Dec 2003). "Presolar diamond, silicon carbide, and graphite in carbonaceous chondrites: Implications for thermal processing in the solar nebula". Geochimica et Cosmochimica Acta. 67 (24): 4823. Bibcode:2003GeCoA..67.4823H. doi:10.1016/j.gca.2003.07.019.
  88. ^ Zinner, E; Amari, S; Guinness, R; Nguyen, A (Dec 2003). "Presolar spinel grains from the Murray and Murchison carbonaceous chondrites". Geochimica et Cosmochimica Acta. 67 (24): 5083. Bibcode:2003GeCoA..67.5083Z. doi:10.1016/S0016-7037(03)00261-8.
  89. ^ Moissan, H (1904). "Investigation of the Canon Diablo Meteorite". Comptes Rendus de l'Académie des Sciences de Paris. 139: 773.
  90. ^ Ksanda, C; Henderson, E (1939). "Identification of diamond in the Canyon Diablo iron". American Mineralogist. 24: 677.
  91. ^ Laspeyres, H; Kaiser, E (1895). "Quartz and Zerkonkrystall im Meteoreisen Toluca von Mexico". Zeitschrift für Krystallographie und Mineralogie. 24: 485.
  92. ^ Bernatowicz, T; Amari, S; Zinner, E; Lewis, R (Jun 1991). "Interstellar Grains within Interstellar Grains". Astrophysical Journal Letters. 373: L73. Bibcode:1991ApJ...373L..73B. doi:10.1086/186054.
  93. ^ Brett, R (1967). "Cohenite: its occurrence and a proposed origin". Geochimica et Cosmochimica Acta. 31 (2): 143. Bibcode:1967GeCoA..31..143B. doi:10.1016/S0016-7037(67)80042-5.
  94. ^ Nagy, B; Andersen, C (1964). "Electron probe microanalysis of some carbonate, sulfate and phosphate minerals in the Orgueil meteorite". American Mineralogist. 49: 1730.
  95. ^ Sofe, M; Lee, M; Lindgren, P; Smith, C (2011). CL Zoning of Calcite in CM Carbonaceous Chondrites and its Relationship to Degree of Aqueous Alteration. 74th Meteoritical Society Meeting.
  96. ^ de Leuw, S; Rubin, A; Wasson, J (Jul 2010). "Carbonates in CM chondrites: Complex formational histories and comparison to carbonates in CI chondrites". Meteoritics & Planetary Science. 45 (4): 513. Bibcode:2010M&PS...45..513D. doi:10.1111/j.1945-5100.2010.01037.x. S2CID 14208785.
  97. ^ Lee, M; Lindgren, P; Sofe, M (Nov 2014). "Aragonite, breunnerite, calcite and dolomite in the CM carbonaceous chondrites: High fidelity recorders of progressive parent body aqueous alteration". Geochimica et Cosmochimica Acta. 144: 126. Bibcode:2014GeCoA.144..126L. doi:10.1016/j.gca.2014.08.019.
  98. ^ Cody, G; Alexander, C (Feb 2005). "NMR studies of chemical structural variation of insoluble organic matter from different carbonaceous chondrite groups". Geochimica et Cosmochimica Acta. 69 (4): 1085. Bibcode:2005GeCoA..69.1085C. doi:10.1016/j.gca.2004.08.031.
  99. ^ Cronin, J Pizzarello S; Frye, J (Feb 1987). "13C NMR spectroscopy of the insoluble carbon of carbonaceous chondrites". Geochimica et Cosmochimica Acta. 51 (2): 299–303. Bibcode:1982Metic..17..200C. doi:10.1016/0016-7037(87)90242-0. PMID 11542083.
  100. ^ Easton, A; Lovering, J (1963). "The analysis of chondritic meteorites". Geochimica et Cosmochimica Acta. 27 (7): 753. Bibcode:1963GeCoA..27..753E. doi:10.1016/0016-7037(63)90040-1.
  101. ^ Moss, A; Hey, M; Elliott, C; Easton, A (Mar 1967). "Methods for the Chemical Analysis of Meteorites II: The major and some minor constituents of chondrites". Mineralogical Magazine. 36 (277): 101. Bibcode:1967MinM...36..101M. doi:10.1180/minmag.1967.036.277.17.
  102. ^ a b Briggs, M; Mamikunian, G (May 1963). "Organic Constituents of the Carbonaceous Chondrites". Space Science Reviews. 1 (4): 57–85. Bibcode:1963SSRv....1..647B. doi:10.1007/BF00212447. PMID 11881656. S2CID 10422212.
  103. ^ Remusat, L; Le Guillou, C; Rouzaud, J; Binet, L; Derenne, S; Robert, F (Jan 2007). "Molecular study of insoluble organic matter in Kainsaz CO3 carbonaceous chondrite: Comparison with CI and CM IOM". Meteoritics & Planetary Science. 43 (7): 1099. doi:10.1111/j.1945-5100.2008.tb01115.x. S2CID 98683674.
  104. ^ Degens, E; Bajor, M (1963). "Amino acids and sugars in the bruderheim and Murray meteorite". Die Naturwissenschaften. 49 (24): 605. doi:10.1007/BF01178050. S2CID 42359207.
  105. ^ Kaplan, I; Degens, E; Reuter, J (Jul 1963). "Organic compounds in stony meteorites". Geochimica et Cosmochimica Acta. 27 (7): 805. Bibcode:1963GeCoA..27..805K. doi:10.1016/0016-7037(63)90045-0.
  106. ^ Kallman Bijl, H, ed. (1960). "Extraterrestrial Life: Some Organic Constituents of Meteorites". Space Research. Amsterdam: North-Holland Publishing Company. p. 1171.
  107. ^ Briggs, M (1961). "Organic constituents of meteorites". Nature. 191 (4794): 1137. Bibcode:1961Natur.191.1137B. doi:10.1038/1911137a0. S2CID 40559837.
  108. ^ Hamilton, P. B. (1965). "Amino acids on hands". Nature. 205 (4968): 284–5. Bibcode:1965Natur.205..284H. doi:10.1038/205284b0. PMID 14270714. S2CID 4189815.
  109. ^ Oró, J; Skewes, H (1965). "Free Amino-Acids on Human Fingers: The Question of Contamination in Microanalysis". Nature. 207 (5001): 1042–5. Bibcode:1965Natur.207.1042O. doi:10.1038/2071042a0. PMID 5866306. S2CID 4275454.
  110. ^ Nuevo, M; Cooper, G; Sandford, S (2018). "Deoxyribose and deoxysugar derivatives from photoprocessed astrophysical ice analogues and comparison to meteorites". Nature Communications. 9 (1): 5276. Bibcode:2018NatCo...9.5276N. doi:10.1038/s41467-018-07693-x. PMC 6299135. PMID 30563961.
  111. ^ Kvenvolden, K; Lawless, J; Pering, K; Peterson, E; Flores, J; Ponnamperuma, C (Dec 1970). "Evidence for Extraterrestrial Amino-acids and Hydrocarbons in the Murchison Meteorite". Nature. 228 (5275): 923–6. Bibcode:1970Natur.228..923K. doi:10.1038/228923a0. PMID 5482102. S2CID 4147981.
  112. ^ Oró, J; Gibert, J; Lichtenstein, H; Wikstrom, S; Flory, D (Mar 1971). "Amino-acids, Aliphatic and Aromatic Hydrocarbons in the Murchison Meteorite". Nature. 230 (5289): 105–6. Bibcode:1971Natur.230..105O. doi:10.1038/230105a0. PMID 4927006. S2CID 4240808.
  113. ^ a b Kvenvolden, K; Lawless, J; Pering, K (Dec 1970). "Evidence for Extraterrestrial Amino-acids and Hydrocarbons in the Murchison Meteorite". Nature. 228 (5275): 923–926. Bibcode:1970Natur.228..923K. doi:10.1038/228923a0. PMID 5482102. S2CID 4147981.
  114. ^ a b Koga, T; H, Naraoka (Apr 2017). "A new family of extraterrestrial amino acids in the Murchison meteorite". Scientific Reports. 7 (1): 636. Bibcode:2017NatSR...7..636K. doi:10.1038/s41598-017-00693-9. PMC 5428853. PMID 28377577.
  115. ^ Mullie, F Reisse J (1987). Organic matter in carbonaceous chondrites, in Topics In Current Chemistry-Series 139. New York: Springer. pp. 83–117.
  116. ^ a b Engel, M; Macko, S (Sep 1997). "Isotopic evidence for extraterrestrial non-racemic amino acids in the Murchison meteorite". Nature. 389 (6648): 265–8. Bibcode:1997Natur.389..265E. doi:10.1038/38460. PMID 9305838. S2CID 4411982.
  117. ^ Elsila, J; Charnley, S; Burton, A; Glavin, D; Dworkin, J (Sep 2012). "Compound‐specific carbon, nitrogen, and hydrogen isotopic ratios for amino acids in CM and CR chondrites and their use in evaluating potential formation pathways". Meteoritics & Planetary Science. 47 (9): 1517. Bibcode:2012M&PS...47.1517E. doi:10.1111/j.1945-5100.2012.01415.x. hdl:2060/20120014482. S2CID 19154600.
  118. ^ Botta, O; Martins, Z; Ehrenfreund, P (Jan 2007). "Amino acids in Antarctic CM1 meteorites and their relationship to other carbonaceous chondrites". Meteoritics & Planetary Science. 42 (1): 81–92. Bibcode:2007M&PS...42...81B. doi:10.1111/j.1945-5100.2007.tb00219.x.
  119. ^ Smith, K; House, C; Arevalo, R; Dworkin, J; Callahan, M (Jun 2019). "Organometallic compounds as carriers of extraterrestrial cyanide in primitive meteorites". Nature Communications. 10 (1): 2777. Bibcode:2019NatCo..10.2777S. doi:10.1038/s41467-019-10866-x. PMC 6592946. PMID 31239434.
  120. ^ Stoks, P; Schwartz, A (Apr 1981). "Nitrogen-heterocyclic compounds in meteorites: significance and mechanisms of formation". Geochimica et Cosmochimica Acta. 45 (4): 563–69. Bibcode:1981GeCoA..45..563S. doi:10.1016/0016-7037(81)90189-7.
  121. ^ Hayatsu, R Anders E (1981). Organic compounds in meteorites and their origins, in Topics in Current Chemistry 99. Berlin, Heidelberg: Springer-Verlag. pp. 1–37. ISBN 978-3-540-10920-4.
  122. ^ Schmitt-Kopplin, P; Gabelica, Z; Gougeon, R (Feb 2010). "High molecular diversity of extraterrestrial organic matter in Murchison meteorite revealed 40 years after its fall". PNAS. 107 (7): 2763–2768. Bibcode:2010PNAS..107.2763S. doi:10.1073/pnas.0912157107. PMC 2840304. PMID 20160129.
  123. ^ Yamashita, Y; Naraoka, H (Jan 2014). "Two homologous series of alkylpyridines in the Murchison meteorite". Geochemical Journal. 48 (6): 519–525. Bibcode:2014GeocJ..48..519Y. doi:10.2343/geochemj.2.0340.
  124. ^ Mueller, G (Aug 1953). "The properties and theory of genesis of the carbonaceous complex within the cold bokevelt meteorite". Geochimica et Cosmochimica Acta. 4 (1–2): 1. Bibcode:1953GeCoA...4....1M. doi:10.1016/0016-7037(53)90061-1.
  125. ^ Engel, M Nagy, B (Apr 1982). "Distribution and enantiomeric composition of amino acids in the Murchison meteorite". Nature. 296 (5860): 837. Bibcode:1982Natur.296..837E. doi:10.1038/296837a0. S2CID 4341990.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  126. ^ Pizzarello, S; Yarnes, C (Aug 2018). "Chiral molecules in space and their possible passage to planetary bodies recorded by meteorites". Earth and Planetary Science Letters. 496: 198. Bibcode:2018E&PSL.496..198P. doi:10.1016/j.epsl.2018.05.026. S2CID 102863818.
  127. ^ a b Pizzarello, S; Yarnes, C (Dec 2018). "The soluble organic compounds of the Mukundpura meteorite: A new CM chondrite fall". Planetary and Space Science. 164: 127. Bibcode:2018P&SS..164..127P. doi:10.1016/j.pss.2018.07.002. S2CID 125844045.
  128. ^ Meierhenrich, U; Muñoz Caro, G; Bredehöft, J; Jessberger, E; Thiemann, W (22 Jun 2004). "Identification of diamino acids in the Murchison meteorite". PNAS. 101 (25): 9182–86. Bibcode:2004PNAS..101.9182M. doi:10.1073/pnas.0403043101. PMC 438950. PMID 15194825.
  129. ^ Martins, Z; Modica, P; Zanda, B; Le Sergeant d'Hendecourt, L (May 2015). "The amino acid and hydrocarbon contents of the Paris meteorite: Insights into the most primitive CM chondrite". Meteoritics & Planetary Science. 50 (5): 926–43. Bibcode:2015M&PS...50..926M. doi:10.1111/maps.12442. hdl:10044/1/25091. S2CID 95549163.
  130. ^ Rudraswami, N; Naik, A; Tripathi, R; Bhandari, N; Karapurkar, S; Prasad, M; Babu, E; Sarathi, V (Feb 2018). "Chemical, isotopic and amino acid composition of Mukundpura CM2.0 (CM1) chondrite: Evidence of parent body aqueous alteration". Geoscience Frontiers. 10 (2): 495–504. doi:10.1016/j.gsf.2018.02.001.
  131. ^ Reynolds, J (Apr 1960). "Isotopic Composition of Primordial Xenon". Phys. Rev. Lett. 4 (7): 351–354. Bibcode:1960PhRvL...4..351R. doi:10.1103/PhysRevLett.4.351.
  132. ^ a b Heymann, D; Mazor, E (May 1967). "Light-Dark Structure and Rare Gas Content of the Carbonaceous Chondrite Nogoya". Journal of Geophysical Research: Atmospheres. 72 (10): 2704–2707. Bibcode:1967JGR....72.2704H. doi:10.1029/JZ072i010p02704.
  133. ^ Wasson, J (1985). Meteorites: Their record of early solar-system history. New York: W. H. Freeman and Co. p. 59. ISBN 978-0716717003.
  134. ^ Goswami, J; Lal, D; Wilkening, L (Jan–Feb 1984). "Title: Gas-rich meteorites - Probes for particle environment and dynamical processes in the inner solar system". Space Science Reviews. 37: 111–159. doi:10.1007/BF00213959. S2CID 121335431.
  135. ^ Lewis, R; Srinivasan, B; Anders, E (26 Dec 1975). "Host Phase of a Strange Xenon Component in Allende". Science. 490 (4221): 1251–1262. Bibcode:1975Sci...190.1251L. doi:10.1126/science.190.4221.1251. S2CID 94192045.
  136. ^ Huss, G; Lewis, R (1994). "Noble gases in presolar diamonds I: Three distinct components and their implications for diamond origins". Meteoritics. 29 (6): 791. Bibcode:1994Metic..29..791H. doi:10.1111/j.1945-5100.1994.tb01094.x.
  137. ^ Bernatowicz, T; Fraundorf, G; Ming, T; Anders, E; Wopenka, B; Zinner, E; Fraundorf, P (1987). "Evidence for interstellar silicon carbide in the Murray carbonaceous meteorite". Nature. 330: 728–730. doi:10.1038/330728a0. S2CID 4361807.
  138. ^ Zinner, E; Ming, T; Anders, E (1987). "Large isotopic anomalies of silicon, carbon, nitrogen, and noble gases in interstellar silicon carbode in the Murray carbonaceous meteorite". Nature. 330: 730. doi:10.1038/330730a0. S2CID 4306270.
  139. ^ Amari, S; Anders, E; Virag, A; Zinner, E (1990). "Interstellar graphite in meteorites". Nature. 345 (6272): 238. Bibcode:1990Natur.345..238A. doi:10.1038/345238a0. S2CID 10272604.
  140. ^ Black, D (Mar 1972). "On the origins of trapped helium, neon and argon isotopic variations in meteorites—II. Carbonaceous meteorites". Geochimica et Cosmochimica Acta. 36 (3): 377–394. Bibcode:1972GeCoA..36..377B. doi:10.1016/0016-7037(72)90029-4.
  141. ^ Füri, E; Aléon-Toppani, A; Marty, B; Libourel, G; Zimmermann, L (Sep 2013). "Effects of atmospheric entry heating on the noble gas and nitrogen content of micrometeorites". Earth and Planetary Science Letters. 377: 1–12. Bibcode:2013E&PSL.377....1F. doi:10.1016/j.epsl.2013.07.031.
  142. ^ Nakamura, T; Noguchi, T; Ozono, Y; Osawa, T; Nagao, K (12 Sep 2005). Mineralogy of Ultracarbonaceous Large Micrometeorites. 68th Meteoritical Society.
  143. ^ Clayton, R; Onuma, N; Grossman, L; Mayeda, T (Mar 1977). "Distribution of the pre-solar component in Allende and other carbonaceous chondrites". Earth and Planetary Science Letters. 32 (2): 209. Bibcode:1977E&PSL..34..209C. doi:10.1016/0012-821X(77)90005-X.
  144. ^ Clayton, R; Mayeda, T (Jul 1999). "Oxygen isotope studies of carbonaceous chondrites". Geochimica et Cosmochimica Acta. 63 (13–14): 2089. Bibcode:1999GeCoA..63.2089C. doi:10.1016/S0016-7037(99)00090-3.
  145. ^ Greenwood, R; Howard, K; Franchi, I; Zolensky, M; Buchanan, P; Gibson, J (Mar 2014). Oxygen Isotope Evidence For The Relationship Between CM And CO Chondrites: Could They Both Coexist On A Single Asteroid?. 45th LPSC.
  146. ^ Hanna, R; Ketcham, R; Zolensky, M; Behr, W (Dec 2015). "Impact-induced brittle deformation, porosity loss, and aqueous alteration in the Murchison CM chondrite". Geochimica et Cosmochimica Acta. 171: 256. Bibcode:2015GeCoA.171..256H. doi:10.1016/j.gca.2015.09.005.
  147. ^ Merrill, G (1921). "On metamorphism in meteorites". Bull. Geol. Soc. Am. 32 (4): 395. Bibcode:1921GSAB...32..395M. doi:10.1130/GSAB-32-395.
  148. ^ Hildebrand, A; McCausland, P; Brown, P; Longstaffe, F; Russell, S; Tagliaferri, E (2006). "The fall and recovery of the Tagish Lake meteorite". Meteoritics & Planetary Science. 41 (3): 407. Bibcode:2006M&PS...41..407H. doi:10.1111/j.1945-5100.2006.tb00471.x.
  149. ^ Flynn, G; Consolmagno, G; Brown, P; Macke, R (Sep 2018). "Physical properties of the stone meteorites: Implications for the properties of their parent bodies". Geochemistry. 78 (3): 269. Bibcode:2018ChEG...78..269F. doi:10.1016/j.chemer.2017.04.002.
  150. ^ Heck, P; Schmitz, B; Bottke, W; Rout, S; Kita, N (Jan 2017). "Rare meteorites common in the Ordovician period". Nature Astronomy. 1 (2): 0035. Bibcode:2017NatAs...1E..35H. doi:10.1038/s41550-016-0035. S2CID 102488048.
  151. ^ Grady, M; Hutchison, R (1998). Meteorites: Flux with Time and Impact Effects. Geological Society of London. pp. 67–70. ISBN 9781862390171. sec. The frequency of meteorite types
  152. ^ Cassidy, W; Rancitelli, L (Mar 1982). "Antarctic Meteorites: The abundant material being discovered in Antarctica may shed light on the evolution of meteorite parent bodies and the history of the solar system". American Scientist. 70 (2): 156–164. JSTOR 27851347.
  153. ^ Lauretta, D; McSween, H, eds. (2006). Meteorites and the Early Solar System II. Tucson: University of Arizona Press. p. 853. ISBN 9780816525621. Ch. Weathering of Chondritic Meteorites, Bland, P., Zolensky, M., Benedix, G., Sephton, M.
  154. ^ Korotev, Randy L. "Some Meteorite Statistics". Department of Earth and Planetary Sciences, Washington University in St. Louis. Washington University in St. Louis. Retrieved 14 Sep 2019.
  155. ^ Encyclopedia of Planetary Science. Encyclopedia of Earth Science Series. Dordrecht: Springer. 1997. p. 486. ISBN 978-0-412-06951-2. Chapter: Meteorite parent bodies, Britt, D., Lebofsky, L.
  156. ^ Cloutis, E; Binzel, R; Gaffey, M (Feb 2014). "Establishing Asteroid–Meteorite Links". Elements. 10: 25. doi:10.2113/gselements.10.1.25.
  157. ^ Lee, M Cohen B King A Greenwood R (Jul 2019). "The diversity of CM carbonaceous chondrite parent bodies explored using Lewis Cliff 85311" (PDF). Geochimica et Cosmochimica Acta. 257: 224–244. Bibcode:2019GeCoA.264..224L. doi:10.1016/j.gca.2019.07.027.
  158. ^ "Asteroids (from the NEAR press kit)". NSSDC. Retrieved 27 Oct 2019.
  159. ^ Orgel, L, ed. (1998). "4 Asteroids and Meteorites". Evaluating the Biological Potential in Samples Returned from Planetary Satellites and Small Solar System Bodies: Framework for Decision Making. Washington DC: National Academy of Sciences National Academy Press. ISBN 978-0-309-06136-0. "it is likely that the C-type asteroids (which are overwhelmingly the most abundant type in the main belt, especially the middle and outer parts) are represented in various meteorite collections by carbonaceous chondrites"
  160. ^ "Asteroids: Structure and composition of asteroids". ESA- Science & Exploration. European Space Agency. Retrieved 27 Oct 2019.
  161. ^ Burbine, T (2016). "Advances in determining asteroid chemistries and mineralogies". Chemie der Erde. 76 (2): 181. Bibcode:2016ChEG...76..181B. doi:10.1016/j.chemer.2015.09.003.
  162. ^ Lantz, C; Clark, B; Barucci, M; Lauretta, D (May 2013). "Evidence for the effects of space weathering spectral signatures on low albedo asteroids". Astronomy and Astrophysics. 554: A138. Bibcode:2013A&A...554A.138L. doi:10.1051/0004-6361/201321593.
  163. ^ Matsuoka, M; Nakamura, T; Kimura, Y; Hiroi, T; Nakamura, R; Okumura, S; Sasaki, S (Mar 2015). "Pulse-laser irradiation experiments of Murchison CM2 chondrite for reproducing space weathering on C-type asteroids". Icarus. 254: 135. Bibcode:2015Icar..254..135M. doi:10.1016/j.icarus.2015.02.029.
  164. ^ Thompson, M; Loeffler, M; Morris, R; Keller, L; Christoffersen, R (Feb 2019). "Spectral and chemical effects of simulated space weathering of the Murchison CM2 carbonaceous chondrite". Icarus. 319: 499. Bibcode:2019Icar..319..499T. doi:10.1016/j.icarus.2018.09.022.
  165. ^ Bland, P; Alard, O; Benedix, G; Kearsley, A (Sep 2005). "Volatile fractionation in the early solar system and chondrule/matrix complementarity". PNAS. 102 (39): 13755–60. Bibcode:2005PNAS..10213755B. doi:10.1073/pnas.0501885102. PMC 1224360. PMID 16174733.
  166. ^ Franchi, I; Greenwood, R; Howard, K; King, A; Lee, M; Anand, M; Findlay, R (2019). Oxygen Isotope Variation Of CM And Related Chondrites: Multiple Parent Bodies Or A Single Heterogeneous Source?. Meteoritical Society Meeting, 2019. p. 6482.
  167. ^ Lipschutz, M; Zolensky, M; Bell, S (Mar 1999). "New Petrographic And Trace Element Data On Thermally MetamorphosedChondrites". Antarctic Meteorite Research. 12: 57–80.
  168. ^ Kigoshi, K; Matsuda, E. Radiocarbon datings of Yamato meteorites. Houston: Lunar and Planetary Institute. pp. 58–60. in International Workshop on Antarctic Meteorites, Annexstad J. et al., eds.
  169. ^ Mueller, G (Apr 1966). "Significance of Inclusions in Carbonaceous Meteorites". Nature. 210 (5032): 151–155. Bibcode:1966Natur.210..151M. doi:10.1038/210151a0. S2CID 4223453.
  170. ^ Zolensky, M; Weisberg, M; Buchanan, P; Mittlefehldt, D (Jul 1996). "Mineralogy of carbonaceous chondrite clasts in HED achondrites and the Moon". Meteoritics & Planetary Science. 31 (4): 518–37. Bibcode:1996M&PS...31..518Z. doi:10.1111/j.1945-5100.1996.tb02093.x.
  171. ^ Herrin, J; Zolensky, M; Cartwright, J; Mittlefehldt, D; Ross, D (Mar 2011). "Carbonaceous Chondrite-Rich Howardites; The Potential For Hydrous Lithologies On The HED Parent". Lunar and Planetary Science Conference (1608). 42nd LPSC: 2806. Bibcode:2011LPI....42.2806H.{{cite journal}}: CS1 maint: location (link)
  172. ^ Martel, L V. "Kaidun--A Meteorite with Everything but the Kitchen Sink". Planetary Science Research Discoveries. Retrieved 6 Oct 2019.

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