The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration

Braukmüller, Ninja; Wombacher, Frank; Hezel, Dominik C.; Escoube, Raphaëlle; Münker, Carsten

doi:10.1016/j.gca.2018.07.023

Cited by 150 publications

(155 citation statements)

References 110 publications

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“…Based on this observation, Wänke and Dreibus (1988) suggested that the Earth consists of two major chemically distinct components. The dominant component was strongly volatile depleted and highly reduced and the second was less volatile depleted and oxidized with nearly chondritic abundances of the volatile elements (e.g., Braukmüller et al 2018Braukmüller et al , 2019. This model was further refined and modified (O'Neill 1991;Albarède 2009;Schönbächler et al 2010; and is consistent with the following scenario: in a first stage highly reduced and volatile element depleted accreted to form proto-Earth, followed by a major chemical differentiation of the body into a metallic core and a silicate mantle.…”

Section: Compositional Constraints On the Building Blocks Of Earthmentioning

confidence: 80%

“…For this reason, several efforts have been made to obtain robust estimates for the abundances of the chemical elements in the Earth as a whole or in the silicate mantle, the volumetrically dominant chemical reservoir of the Earth (e.g., McDonough and Sun 1995;Allègre et al 1999;Palme and Jones 2003;Palme and O'Neill 2014). These estimates can be compared with bulk analyses made to obtain the absolute element abundance for each meteorite class (e.g., Wasson and Kallemeyn 1988;Miyamoto et al 2016;Clay et al 2017;Braukmüller et al 2018Braukmüller et al , 2019 (Fig. 1).…”

Section: Compositional Constraints On the Building Blocks Of Earthmentioning

confidence: 99%

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Accretion of the Earth—Missing Components?

2020

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Primitive meteorites preserve the chemical and isotopic composition of the first aggregates that formed from dust and gas in the solar nebula during the earliest stages of solar system evolution. Gradual increase in the size of solid bodies from dust to aggregates and then to planetesimals finally led to the formation of planets within a few to tens of million years after the start of condensation. Thus the rocky planets of the inner solar system are likely the result of the accumulation of numerous smaller primitive as well as differentiated bodies. The chemically most primitive known meteorites are chondrites and they consist mostly of metal and silicates. Chondritic meteorites are derived from distinct primitive planetary bodies that experienced only limited element fractionation during formation and subsequent differentiation. Different chondrite classes show distinct chemical and isotopic characteristics, which may reflect heterogeneities in the solar nebula and the slightly different pathways of their formation. To a first approximation the chemical composition of the bulk Earth bears great similarities to primitive meteorites. However, for some elements there are striking and significant differences. The Earth shows a much stronger depletion of the moderate to highly volatile elements compared to chondrites. In addition, mixing trends of specific isotopes reveal that the Earth is most enriched in s-process isotopes compared to all other analysed bulk solar system materials. It is currently not possible to fully define and quantify the different chemical and isotopic materials that formed the Earth, because a major component seems missing in the extant collections of extraterrestrial samples. Variations in nucleosynthetic isotope compositions as well as the strong depletion of moderately and strongly volatile elements points towards a source in the inner solar system for this missing material. It is conceivable that Venus and Mercury contain a much larger fraction of this

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Section: Compositional Constraints On the Building Blocks Of Earthmentioning

confidence: 80%

Section: Compositional Constraints On the Building Blocks Of Earthmentioning

confidence: 99%

Accretion of the Earth—Missing Components?

2020

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“…Barrat et al (2012) is the most complete source of trace element data for Ivuna, although it does not include the abundances of Mo, Ag, Cd, Sn, Sb, and Tl. However, these (and other) trace elements were reported by Greenland (1967), Case et al (1973), Krähenbühl et al (1973), Ebihara et al (1982), Rocholl and Jochum (1993), and Braukmüller et al (2018). None of the trace element abundances in the literature were found to be outliers according to Grubbs' test except for the Cd and Ag measurements of Greenland (1967).…”

Section: Rare Earth Elementsmentioning

confidence: 82%

“…Along with Barrat et al (2012), REE abundances (La -Lu, note Sc and Y are listed as Trace Elements in Table 1) in Ivuna have previously been reported by Schmitt et al (1964), Rocholl and Jochum (1993), Pourmand et al (2012), and Braukmüller et al (2018). The REE abundance patterns given by Schmitt et al (1964) and Rocholl and Jochum (1993) are erratic, probably due to insufficient precision of the analytical technique used in those studies, and those La -Lu datasets were excluded in calculating the average REE abundances of Ivuna.…”

Section: Rare Earth Elementsmentioning

confidence: 99%

“…Apart from Li (off-scale, photospheric abundance a factor of 166 less than Ivuna), the main differences are for Ag (Z = 47) and Pb (Z = 82). and Palme (2001), Wiik (1956), Case et al (1973), Krähenbühl et al (1973), Ebihara et al (1982), Rochol and Jochum (1993), Schmitt et al 4 (1964), Pourmand et al (2012), Kaushal and Wetherill (1970) and Braukmüller et al (2018). LOQ = limit of quantification; S.D.…”

Section: Comparison Between Our Average Ivuna Composition and The Mosmentioning

confidence: 99%

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Terrestrial modification of the Ivuna meteorite and a reassessment of the chemical composition of the CI type specimen

King

Phillips

Strekopytov

et al. 2020

Geochimica et Cosmochimica Acta

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The rare CI carbonaceous chondrites are the most aqueously altered and chemically primitive meteorites but due to their porous nature and high abundance of volatile elements are susceptible to terrestrial weathering. The Ivuna meteorite, type specimen for the CI chondrites, is the largest twentieth-century CI fall and probably the CI chondrite least affected by terrestrial alteration that is available for study. The main mass of Ivuna (BM2008 M1) has been stored in a nitrogen atmosphere at least since its arrival at the Natural History Museum (NHM), London, in 2008 (70 years after its fall) and could be considered the most pristine CI chondrite stone. We report the mineralogy, petrography and bulk elemental composition of BM2008 M1 and a second Ivuna stone (BM1996 M4) stored in air within wooden cabinets. We find that both Ivuna stones are breccias consisting of multiple rounded, phyllosilicate-rich clasts that formed through aqueous alteration followed by impact processing. A polished thin section of BM2008 M1 analysed immediately after preparation was found to contain sulphate-bearing veins that

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Planetary Protection: Too Late

Safonova

Sivaram

2021

Planet Formation and Panspermia

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The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration

Cited by 150 publications

References 110 publications

Accretion of the Earth—Missing Components?

Accretion of the Earth—Missing Components?

Terrestrial modification of the Ivuna meteorite and a reassessment of the chemical composition of the CI type specimen

Planetary Protection: Too Late

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