Highly volatile element (H, C, F, Cl, S) abundances and H isotopic compositions in chondrules from carbonaceous and ordinary chondrites

Shimizu, K.; Alexander, C. M. O'd.; Hauri, E. H.; Sarafian, Adam R.; Nittler, L. R.; Wang, Jingyuan; Jacobsen, S. D.; Mendybaev, R. A.

doi:10.1016/j.gca.2021.03.005

Cited by 15 publications

(9 citation statements)

References 114 publications

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“…The water contents of pyroxene minerals in OC falls (176-868 ppm) are comparable to those of the returned Itokawa pyroxene minerals (278-988 ppm, Jin & Bose 2019; Chan et al 2021), yet the upper limit (868 ppm) is lower than that observed in several pyroxenes from the Type 3 OC Bishunpur (1796 ppm, Stephant et al 2017). In contrast, our results are all higher than the reported water content of one pyroxene grain from the Type 3.05 OC QUE 97008 (12 ppm, Shimizu et al 2021).…”

Section: Water Contentssupporting

confidence: 48%

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New evidence for wet accretion of inner solar system planetesimals from meteorites Chelyabinsk andBenenitra

Jin¹,

Bose²,

Lichtenberg³

et al. 2021

Preprint

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We investigated the hydrogen isotopic compositions and water contents of pyroxenes in two recent ordinary chondrite falls, namely, Chelyabinsk (2013 fall) and Benenitra (2018 fall), and compared them to three ordinary chondrite Antarctic finds, namely Graves Nunataks GRA 06179, Larkman Nunatak LAR 12241, and Dominion Range DOM 10035. The pyroxene minerals in Benenitra and Chelyabinsk are hydrated (∼0.018-0.087 wt.% H 2 O) and show D-poor isotopic signatures (δD SM OW from -444 to -49 ). On the contrary, the ordinary chondrite finds exhibit evidence of terrestrial contamination with elevated water contents (∼0.039-0.174 wt.%) and δD SM OW values (from -199 to -14 ). We evaluated several small parent body processes that are likely to alter the measured compositions in Benenitra and Chelyabinsk, and inferred that water-loss in S-type planetesimals is minimal during thermal metamorphism. Benenitra and Chelyabinsk hydrogen compositions reflect a mixed component of D-poor nebular hydrogen and water from the D-rich mesostases. 45-95% of water in the minerals characterized by low δD SM OW values was contributed by nebular hydrogen. Stype asteroids dominantly composed of nominally anhydrous minerals can hold 254-518 ppm of water. Addition of a nebular water component to nominally dry inner Solar System bodies during accretion suggests a reduced need of volatile delivery to the terrestrial planets during late accretion.

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Section: Water Contentssupporting

confidence: 48%

“…Large variations in water contents of the chondrule mesostases from type 3 OCs (Bishunpur and Semarkona) have been reported (0.0008-1.51 wt.%, Fig. 5, Stephant et al 2017;Shimizu et al 2021). The δD SM OW values of this water range from -166 to 15000 (Stephant et al 2017;Shimizu et al 2021).…”

Section: Major Element Abundancesmentioning

confidence: 93%

New evidence for wet accretion of inner solar system planetesimals from meteorites Chelyabinsk andBenenitra

Jin¹,

Bose²,

Lichtenberg³

et al. 2021

Preprint

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“…Rather than the dehydration of NAMs under high temperatures, NAMs could have received a fraction of water from the interstitial mesostases or matrix, as the latter components of unequilibrated chondrites can contain considerable amounts of water. Large variations in water contents of the chondrule mesostases from type 3 OCs (Bishunpur and Semarkona) have been reported (0.0008-1.51 wt.%; Figure 5; Stephant et al 2017;Shimizu et al 2021). The δD SMOW values of this water range from −166‰ to 15,000‰ (Stephant et al 2017;Shimizu et al 2021).…”

Section: A Source Of Low D/h Ratios In Benenitra and Chelyabinskmentioning

confidence: 93%

“…Large variations in water contents of the chondrule mesostases from type 3 OCs (Bishunpur and Semarkona) have been reported (0.0008-1.51 wt.%; Figure 5; Stephant et al 2017;Shimizu et al 2021). The δD SMOW values of this water range from −166‰ to 15,000‰ (Stephant et al 2017;Shimizu et al 2021). Besides, δD SMOW values of the phyllosilicate in the matrix of the type 3 OC Semarkona have a large range, and the upper limit can be up to ∼10,000‰ (Figure 5; Piani et al 2015).…”

Section: A Source Of Low D/h Ratios In Benenitra and Chelyabinskmentioning

confidence: 97%

New Evidence for Wet Accretion of Inner Solar System Planetesimals from Meteorites Chelyabinsk and Benenitra

Jin¹,

Bose²,

Lichtenberg³

et al. 2021

Planet. Sci. J.

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We investigated the hydrogen isotopic compositions and water contents of pyroxenes in two recent ordinary chondrite falls, namely, Chelyabinsk (2013 fall) and Benenitra (2018 fall), and compared them to three ordinary chondrite Antarctic finds, namely, Graves Nunataks GRA 06179, Larkman Nunatak LAR 12241, and Dominion Range DOM 10035. The pyroxene minerals in Benenitra and Chelyabinsk are hydrated (∼0.018–0.087 wt.% H2O) and show D-poor isotopic signatures (δDSMOW from −444‰ to −49‰). On the contrary, the ordinary chondrite finds exhibit evidence of terrestrial contamination with elevated water contents (∼0.039–0.174 wt.%) and δDSMOW values (from −199‰ to −14‰). We evaluated several small parent-body processes that are likely to alter the measured compositions in Benenitra and Chelyabinsk and inferred that water loss in S-type planetesimals is minimal during thermal metamorphism. Benenitra and Chelyabinsk hydrogen compositions reflect a mixed component of D-poor nebular hydrogen and water from the D-rich mesostases. A total of 45%–95% of water in the minerals characterized by low δDSMOW values was contributed by nebular hydrogen. S-type asteroids dominantly composed of nominally anhydrous minerals can hold 254–518 ppm of water. Addition of a nebular water component to nominally dry inner solar system bodies during accretion suggests a reduced need of volatile delivery to the terrestrial planets during late accretion.

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“…However, sulfide condensation is predicted to increase with increasing total pressure and dust/gas ratio and will start at almost 1400 K at P = 10 −3 bars and dust/gas = 1000 times solar (Ebel & Grossman, 2000). There is also evidence that at least some type I chondrule mesostases reached sulfide saturation prior to solidifying (Marrocchi & Libourel, 2013;Shimizu et al, 2021). Many type II chondrules probably achieved sulfide saturation before solidifying.…”

Section: Clues From S Isotopesmentioning

confidence: 99%

Sulfur abundances and isotopic compositions in bulk carbonaceous chondrites and insoluble organic material: Clues to elemental and isotopic fractionations of volatile chalcophiles

Alexander

Wynn

Bowden

2021

Meteorit & Planetary Scien

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The bulk S elemental abundances and δ 34 S values for 83 carbonaceous chondrites (mostly CMs and CRs) and Semarkona (LL3.0) are reported. In addition, the S elemental abundances and δ 34 S values of insoluble organic material (IOM) isolated from 25 carbonaceous chondrites (CMs, CRs, and three ungrouped) are presented. The IOM only contributes 2-7% of the S to the bulk meteorites analyzed and exhibits no systematic variations. The average group bulk S abundances are similar to previous measurements. Ingroup variations likely reflect variations in matrix abundances, as well as parent body processes and weathering. The S and C abundances are roughly correlated and scatter about a mixing line between CI-like matrix and C-free and S-depleted chondrules. Systematic deviations from this mixing line may indicate different degrees of heating of matrix material in the nebula. There are no systematic variations in average group δ 34 S values, in contrast to what is seen for the volatile chalcophiles Zn, Te, Se, and Ag, as well as the less volatile siderophile Cu. Renormalization of the elemental and isotopic compositions indicates that the elemental and isotopic fractionations of Zn, Te, and Ag were controlled by the same process, whereas Se is intermediate in its behavior between these three elements and S. The isotopic fractionations could be associated with diffusion of volatile chalcophiles into sulfide at the end of chondrule formation. Copper appears to be distinct in its behavior from the chalcophiles, perhaps because it is more refractory and more siderophile.

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Highly volatile element (H, C, F, Cl, S) abundances and H isotopic compositions in chondrules from carbonaceous and ordinary chondrites

Cited by 15 publications

References 114 publications

New evidence for wet accretion of inner solar system planetesimals from meteorites Chelyabinsk andBenenitra

New evidence for wet accretion of inner solar system planetesimals from meteorites Chelyabinsk andBenenitra

New Evidence for Wet Accretion of Inner Solar System Planetesimals from Meteorites Chelyabinsk and Benenitra

Sulfur abundances and isotopic compositions in bulk carbonaceous chondrites and insoluble organic material: Clues to elemental and isotopic fractionations of volatile chalcophiles

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