Sulfur isotope signatures of eucrites and diogenites

Wu, Nanping; Farquhar, James; Dottin, James W.; Magalhães, Nívea

doi:10.1016/j.gca.2018.05.002

Cited by 14 publications

(29 citation statements)

References 77 publications

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“…One possibility is that the sulfur-rich medium might have formed due to degassing of a sulfur-bearing magma during its intrusion 25,29 . Degassing of sulfur has been suggested based on the presence of 34 S enrichment in some eucrite meteorites 40 and consideration on the depletion of volatile siderophile elements in eucrites 41 .…”

Section: Discussionmentioning

confidence: 99%

Evidence of metasomatism in the interior of Vesta

et al. 2020

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Diogenites are a group of meteorites that are derived from the interior of the largest protoplanet Vesta. They provide a unique opportunity to understanding together the internal structure and dynamic evolution of this protoplanet. Northwest Africa (NWA) 8321 was suggested to be an unbrecciated noritic diogenite meteorite, which is confirmed by our oxygen and chromium isotopic data. Here, we find that olivine in this sample has been partly replaced by orthopyroxene, troilite, and minor metal. The replacement texture of olivine is unambiguous evidence of sulfur-involved metasomatism in the interior of Vesta. The presence of such replacement texture suggests that in NWA 8321, the olivine should be of xenolith origin while the noritic diogenite was derived from partial melting of pre-existing rocks and had crystallized in the interior of Vesta. The post-Rheasilvia craters in the northpolar region on Vesta could be the potential source for NWA 8321.

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Section: Discussionmentioning

confidence: 99%

Evidence of metasomatism in the interior of Vesta

et al. 2020

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“…Consideration of S‐poor and S‐rich vestan core also does not influence this fundamental pattern; we have modeled both a 15 wt% S core and a 0.5 wt% S core, the latter derived from S contents in eucrites measured by Wu et al. () and assuming sulfide undersaturation for the eucritic liquids. This mismatch suggests either that the volatile depletions have been overestimated, or that most VSE were added to the vestan mantle after core formation.…”

Section: Vse Concentrations In Silicate Mantlesmentioning

confidence: 99%

Effect of silicon on activity coefficients of Bi, Cd, Sn, and Ag in liquid Fe‐Si, and implications for differentiation and core formation

Righter¹,

Pando

Ross

et al. 2019

Meteorit & Planetary Scien

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The depletion of volatile siderophile elements (VSE) Sn, Ag, Bi, Cd, and P in mantles of differentiated planetary bodies can be attributed to volatile‐depleted precursor materials (building blocks), fractionation during core formation, fractionation into and retention in sulfide minerals, and/or volatile loss associated with magmatism. Quantitative models to constrain the fractionation due to core formation have not been possible due to the lack of activity and partitioning data. Interaction parameters in Fe‐Si liquids have been measured at 1 GPa, 1600 °C and increase in the order Cd (~6), Ag (~10), Sn (~28), Bi (~46), and P (~58). These large and positive values contrast with smaller and negative values in Fe‐S liquids indicating that any chalcophile behavior exhibited by these elements will be erased by dissolution of a small amount of Si in the metallic liquid. A newly updated activity model is applied to Earth, Mars, and Vesta. Five elements (P, Zn, Sn, Cd, and In) in Earth's primitive upper mantle can largely be explained by metal‐silicate equilibrium at high PT conditions where the core‐forming metal is a Fe‐Ni‐S‐Si‐C metallic liquid, but two other—Ag and Bi—become overabundant during core formation and require a removal mechanism such as late sulfide segregation. All of the VSE in the mantle of Mars are consistent with core formation in a volatile element depleted body, and do not require any additional processes. Only P and Ag in Vesta's mantle are consistent with combined core formation and volatile‐depleted precursors, whereas the rest require accretion of chondritic or volatile‐bearing material after core formation. The concentrations of Zn, Ag, and Cd modeled for Vesta's core are similar to the concentration range measured in magmatic iron meteorites indicating that these volatile elements were already depleted in Vesta's precursor materials.

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“…An important observation from our work and that presented in Wing and Farquhar (2015) is that the   S values of mare basalts is no different than that of the silicate Earth (where   S = 0‰, Labidi et al 2013). Recent work has shown that various primitive and differentiated meteoritic materials have distinct   S compositions that are linked to specific parent bodies where the differences in   S among the parent bodies may be due to processing of sulfur in different nebular environments (Antonelli et al, 2014;Dottin III et al, 2018;Labidi et al, 2017;Rai et al, 2005;Wu et al, 2018). Furthermore, similarity in   S between various planetary materials (e.g.…”

Section: Implications For the   S Values Of Mare Basaltsmentioning

confidence: 50%

“…In total, these data provide further evidence for the idea that lunar volatile loss and volatile-element stable isotope fractionation largely occurred during lunar formation and that exceptionally high or low isotopic compositions likely resulted from localized phenomena influenced by reservoir effects. Faircloth et al, 2020;Gao and Thiemens, 1991;Gao and Thiemens, 1993a;Gao and Thiemens, 1993b;Labidi et al, 2013;Rees and Thode, 1974;Saal and Hauri, 2021;Wing and Farquhar, 2015;Wu et al, 2018). Green bar represents the estimated  34 S value of the silicate Earth (Labidi et al, 2013).…”

Section: Discussionmentioning

confidence: 99%

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The Zn, S, and Cl isotope compositions of mare basalts: Implications for the effects of eruption style and pressure on volatile element stable isotope fractionation on the Moon

Gargano

Dottin

Hopkins

et al. 2022

American Mineralogist

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We compare the stable isotope compositions of Zn, S, and Cl for Apollo mare basalts to better constrain the sources and timescales of lunar volatile loss. Mare basalts have broadly elevated yet limited ranges in δ66Zn, δ34S, and δ37ClSBC+WSC values of 1.27 ± 0.71, 0.55 ± 0.18, and 4.1 ± 4.0‰, respectively, compared to the silicate Earth at 0.15, –1.28, and 0‰, respectively. We find that the Zn, S, and Cl isotope compositions are similar between the low- and high-Ti mare basalts, providing evidence of a geochemical signature in the mare basalt source region that is inherited from lunar formation and magma ocean crystallization. The uniformity of these compositions implies mixing following mantle overturn, as well as minimal changes associated with subsequent mare magmatism. Degassing of mare magmas and lavas did not contribute to the large variations in Zn, S, and Cl isotope compositions found in some lunar materials (i.e., 15‰ in δ66Zn, 60‰ in δ34S, and 30‰ in δ37Cl). This reflects magma sources that experienced minimal volatile loss due to high confining pressures that generally exceeded their equilibrium saturation pressures. Alternatively, these data indicate effective isotopic fractionation factors were near unity. Our observations of S isotope compositions in mare basalts contrast to those for picritic glasses (Saal and Hauri 2021), which vary widely in S isotope compositions from –14.0 to 1.3‰, explained by extensive degassing of picritic magmas under high-P/PSat values (>0.9) during pyroclastic eruptions. The difference in the isotope compositions of picritic glass beads and mare basalts may result from differences in effusive (mare) and explosive (picritic) eruption styles, wherein the high-gas contents necessary for magma fragmentation would result in large effective isotopic fractionation factors during degassing of picritic magmas. Additionally, in highly vesiculated basalts, the δ34S and δ37Cl values of apatite grains are higher and more variable than the corresponding bulk-rock values. The large isotopic range in the vesiculated samples is explained by late-stage low-pressure “vacuum” degassing (P/PSat ~ 0) of mare lavas wherein vesicle formation and apatite crystallization took place post-eruption. Bulk-rock mare basalts were seemingly unaffected by vacuum degassing. Degassing of mare lavas only became important in the final stages of crystallization recorded in apatite—potentially facilitated by cracks/fractures in the crystallizing flow. We conclude that samples with wide-ranging volatile element isotope compositions are likely explained by localized processes, which do not represent the bulk Moon.

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Sulfur isotope signatures of eucrites and diogenites

Cited by 14 publications

References 77 publications

Evidence of metasomatism in the interior of Vesta

Evidence of metasomatism in the interior of Vesta

Effect of silicon on activity coefficients of Bi, Cd, Sn, and Ag in liquid Fe‐Si, and implications for differentiation and core formation

The Zn, S, and Cl isotope compositions of mare basalts: Implications for the effects of eruption style and pressure on volatile element stable isotope fractionation on the Moon

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