Noble gas record, collisional history, and pairing of CV, CO, CK, and other carbonaceous chondrites

Scherer, P.; Schultz, L.

doi:10.1111/j.1945-5100.2000.tb01981.x

Cited by 92 publications

(123 citation statements)

References 22 publications

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“…The exposure ages of CV and CK chondrites show comparable patterns, with two clusters developed at ~9 and ~29 Ma (Scherer and Schultz, 2000). In comparison, CO chondrite exposure ages extend to higher values than either the CVs and CKs, whereas CI and CM chondrites are much lower, being generally less than 7 Ma (Scherer and Schultz, 2000).…”

Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 66%

“…In comparison, CO chondrite exposure ages extend to higher values than either the CVs and CKs, whereas CI and CM chondrites are much lower, being generally less than 7 Ma (Scherer and Schultz, 2000). Scherer and Schultz (2000) suggest that the similarity in their cosmic-ray exposure age distributions supports a close relationship between CV and CK chondrites.…”

Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 90%

“…One means of examining whether CVs and CKs could have come from a common parent body is to look at their cosmic-ray exposure age distributions (Scherer and Schultz, 2000). The exposure ages of CV and CK chondrites show comparable patterns, with two clusters developed at ~9 and ~29 Ma (Scherer and Schultz, 2000).…”

Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 99%

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The relationship between CK and CV chondrites

Greenwood¹,

Franchi²,

Kearsley³

et al. 2010

Geochimica et Cosmochimica Acta

104

195

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CK chondrites are highly oxidized meteorites containing abundant magnetite and trace amounts of Fe,Ni-metal. Although the group is predominately composed of equilibrated meteorites (types 4 to 6), in recent years a significant number of new samples have been classified as being either CK3 or CK3-anomalous. These unequilibrated CKs often display a close affinity with members of the CV oxidized subgroup. CKs and CVs (oxidized subgroup) may therefore form a continuum and by implication could be derived from a single common parent body. To investigate the relationship between these two groups a detailed study of the oxygen isotope composition, opaque mineralogy and major and trace element geochemistry of a suite of CV and CK chondrites has been undertaken. The results of oxygen isotope analysis confirm the close affinity between CV and CK chondrites, while excluding the possibility of a linkage between the CO and CK groups. Magnetites in both CV and CK chondrites show significant compositional similarities, but high Ti contents are a diagnostic feature of the latter group. The results of major and trace element analysis demonstrate that both CV and CK chondrites show overlapping variation. Supporting evidence for a single common source for both groups comes from their similar cosmic-ray exposure age distributions. Recent reflectance spectral analysis is consistent with both the CVs and CKs being derived from Eos family asteroids, which are believed to have formed by the catastrophic disruption of a single large asteroid. Thus, a range of evidence appears to be consistent with CV and CK chondrites representing samples from a single thermally stratified parent body. In view of the close similarity between CV and CK chondrites some modification of the present classification scheme may be warranted, possibly involving integration of the two groups. One means of achieving this would be to reassigned CK chondrites to a subgroup of the oxidized CVs. It is recognized that a full evaluation of this proposal may require further study of the still poorly understood CK3 chondrites. ACCEPTED MANUSCRIPT3

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Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 66%

Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 90%

Section: Ck and CV Chondrites: How Many Parent Bodies?mentioning

confidence: 99%

See 1 more Smart Citation

The relationship between CK and CV chondrites

Greenwood¹,

Franchi²,

Kearsley³

et al. 2010

Geochimica et Cosmochimica Acta

104

195

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“…The concentration of 3 He in this mantle reservoir can be estimated if we assume a closed system, BSE UCTh, an initial 3 He/ 4 He of 120R a and a present-day 3 He/ 4 He similar to the maximum observed in plumes of 50R a , which is approximately 100 times the 3 He concentration of the convecting mantle itself (e.g. Porcelli & Wasserburg 1995 Mazor et al (1970) and Scherer & Schultz (2000)). As discussed earlier, Xe isotopes require that we must allow for at least a 100-fold loss of noble gases during the accretionary process .…”

Section: Support For Subducted 'Air' Noble Gases In the Terrestrial Mmentioning

confidence: 99%

“…Also, the Ne/Xe ratio observed in the highest-concentration meteorites is similar to accretionary Ne/Xe in the terrestrial mantle (horizontal dot-dashed line). Carbonaceous chondrite (CC) data (diamonds, CC type 1; squares, CC type 2; triangles, CC type 3; circles, CC type 4) from Mazor et al (1970) and Scherer & Schultz (2000).…”

Section: Xenon: Massive Early Planetary Volatile Loss and Fractionationmentioning

confidence: 99%

What CO ₂ well gases tell us about the origin of noble gases in the mantle and their relationship to the atmosphere

Ballentine

Holland²

2008

Phil. Trans. R. Soc. A.

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Study of commercially produced volcanic CO 2 gas associated with the Colorado Plateau, USA, has revealed substantial new information about the noble gas isotopic composition and elemental abundance pattern of the mantle. Combined with published data from midocean ridge basalts, it is now clear that the convecting mantle has a maximum 20 Ne/ 22 Ne isotopic composition, indistinguishable from that attributed to solar wind-implanted (SWI) neon in meteorites. This is distinct from the higher 20 Ne/ 22 Ne isotopic value expected for solar nebula gases. The non-radiogenic xenon isotopic composition of the well gases shows that 20 per cent of the mantle Xe is 'solar-like' in origin, but cannot resolve the small isotopic difference between the trapped meteorite 'Q'-component and solar Xe. The mantle primordial 20 Ne/ 132 Xe is approximately 1400 and is comparable with the upper end of that observed in meteorites. Previous work using the terrestrial 129 I-129 Xe mass balance demands that almost 99 per cent of the Xe (and therefore other noble gases) has been lost from the accreting solids and that Pu-I closure age models have shown this to have occurred in the first ca 100 Ma of the Earth's history. The highest concentrations of Q-Xe and solar wind-implanted (SWI)-Ne measured in meteorites allow for this loss and these high-abundance samples have a Ne/Xe ratio range compatible with the 'recycled-aircorrected' terrestrial mantle. These observations do not support models in which the terrestrial mantle acquired its volatiles from the primary capture of solar nebula gases and, in turn, strongly suggest that the primary terrestrial atmosphere, before isotopic fractionation, is most probably derived from degassed trapped volatiles in accreting material.By contrast, the non-radiogenic argon, krypton and 80 per cent of the xenon in the convecting mantle have the same isotopic composition and elemental abundance pattern as that found in seawater with a small sedimentary Kr and Xe admix. These mantle heavy noble gases are dominated by recycling of air dissolved in seawater back into the mantle. Numerical simulations suggest that plumes sampling the core-mantle boundary would be enriched in seawater-derived noble gases compared with the convecting mantle, and therefore have substantially lower 40 Ar/ 36 Ar. This is compatible with observation. The subduction process is not a complete barrier to volatile return to the mantle.

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Cosmic Ray Exposure History of Meteorites

Wieler

Graf

2001

Accretion of Extraterrestrial Matter Throughout Earth’s History

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Noble gas record, collisional history, and pairing of CV, CO, CK, and other carbonaceous chondrites

Cited by 92 publications

References 22 publications

The relationship between CK and CV chondrites

The relationship between CK and CV chondrites

What CO ₂ well gases tell us about the origin of noble gases in the mantle and their relationship to the atmosphere

Cosmic Ray Exposure History of Meteorites

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Noble gas record, collisional history, and pairing of CV, CO, CK, and other carbonaceous chondrites

Cited by 92 publications

References 22 publications

The relationship between CK and CV chondrites

The relationship between CK and CV chondrites

What CO 2 well gases tell us about the origin of noble gases in the mantle and their relationship to the atmosphere

Cosmic Ray Exposure History of Meteorites

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What CO ₂ well gases tell us about the origin of noble gases in the mantle and their relationship to the atmosphere