Carbon isotopic variation in ureilites: Evidence for an early, volatile-rich Inner Solar System

Barrat, Jean‐Alix; Sansjofre, Pierre; Yamaguchi, A.; Greenwood, R. C.; Gillet, Philippe

doi:10.1016/j.epsl.2017.08.039

Cited by 27 publications

(32 citation statements)

References 43 publications

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“…Thus, our results show that the diamonds in the ureilites could be formed from the different sources under various conditions of synthesis and metamorphism and could represent several generations in a single meteorite. Isotopic evidences for two sources of carbon in the ureilites (Barrat et al 2017) and textural signs of post-igneous addition of carbon into the ureilite suggested by Day et al (2017) seem to be in agreement with this proposition. Based on the noble gases of the ureilitic carbon phases, it was suggested that ureilitic diamonds should be formed by shock from several sources with variable content of noble gases in a sequence of parent body processes (Le Guillou et al 2010).…”

Section: Interpretation Of the Metamorphism Effect On Diamond Pl Featsupporting

confidence: 73%

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Metamorphism of four desert ureilites and luminescence spectroscopy of defects in ureilitic diamonds

Lorenz

Shiryaev

Власов

et al. 2019

Meteorit & Planetary Scien

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Four ureilites subjected to impact metamorphism in a pressure range of ~15–100 GPa were investigated for mineralogical and petrological features and optical luminescence of their diamonds with the aim to understand how properties of ureilitic diamonds are correlated with shock and thermal histories of the host meteorite. Petrological data show that all the investigated ureilites experienced multistage metamorphic histories. Some of them were shocked at least twice or/and underwent high‐temperature thermal metamorphism and fluid metasomatism in the parent body interior. Photoluminescence spectra of individual diamond grains reveal the presence of neutral and negatively charged nitrogen‐vacancy (NV0 and NV−, respectively) and H3 (two nitrogens and a vacancy) defects, indicating relatively high nitrogen contents of the diamonds and some degree of thermal annealing of the grains. The diamond grain size and morphology, a texture of graphite‐diamond aggregates, and spectroscopic properties of the diamond phase vary widely both within an individual meteorite and between the ureilites. Shock‐driven transformation of sp2‐C into diamond provides the most natural explanation of the observed spectroscopic diversity of the diamond grains if one takes into account strong dependence of the PT parameters and efficiency of the transformation on structure of the carbonaceous precursor.

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Section: Interpretation Of the Metamorphism Effect On Diamond Pl Featsupporting

confidence: 73%

“…Isotopic evidences for two sources of carbon in the ureilites (Barrat et al. ) and textural signs of post‐igneous addition of carbon into the ureilite suggested by Day et al. () seem to be in agreement with this proposition.…”

Section: Discussionsupporting

confidence: 55%

Metamorphism of four desert ureilites and luminescence spectroscopy of defects in ureilitic diamonds

Lorenz

Shiryaev

Власов

et al. 2019

Meteorit & Planetary Scien

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“…There is little doubt that the UPB accreted from isotopically heterogeneous materials. The fact that C (Barrat et al 2017), Cr (Zhu et al 2020), and O isotopes (Clayton and Mayeda 1988) all correlate with the Mg# of silicates suggests that the intrinsic f O 2 of ureilites was at least partly inherited from the precursor chondritic materials. The origin of the intrinsic f O 2 of meteorite parent bodies is an active area of research.…”

Section: Discussionmentioning

confidence: 99%

“…The forsterite content of olivine cores (Fo, equivalent to the Mg#) varies between 74 and 96 with increasing 16 O contents. In addition, ureilites are characterized by heterogeneities in C (Barrat et al 2017), Cr (Van Kooten et al 2017; Zhu et al 2020), and noble gas isotopes (Broadley et al 2020), which also appear to correlate with O isotope compositions.…”

Section: Introductionmentioning

confidence: 99%

Incremental melting in the ureilite parent body: Initial composition, melting temperatures, and melt compositions

Collinet

Grove

2020

Meteorit & Planetary Scien

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Ureilites are carbon-rich ultramafic achondrites that have been heated above the silicate solidus, do not contain plagioclase, and represent the melting residues of an unknown planetesimal (i.e., the ureilite parent body, UPB). Melting residues identical to pigeonite-olivine ureilites (representing 80% of ureilites) have been produced in batch melting experiments of chondritic materials not depleted in alkali elements relative to the Sun's photosphere (e.g., CI, H, LL chondrites), but only in a relatively narrow range of temperature (1120°C-1180°C). However, many ureilites are thought to have formed at higher temperature (1200°C-1280°C). New experiments, described in this study, show that pigeonite can persist at higher temperature (up to 1280°C) when CI and LL chondrites are melted incrementally and while partial melts are progressively extracted. The melt productivity decreases dramatically after the exhaustion of plagioclase with only 5-9 wt% melt being generated between 1120°C and 1280°C. The relative proportion of pyroxene and olivine in experiments is compared to 12 ureilites, analyzed for this study, together with ureilites described in the literature to constrain the initial Mg/Si ratio of the UPB (0.98-1.05). Experiments are also used to develop a new thermometer based on the partitioning of Cr between olivine and low-Ca pyroxene that is applicable to all ureilites. The equilibration temperature of ureilites increases with decreasing Al 2 O 3 and Wo contents of pyroxene and decreasing bulk REE concentrations. The UPB melted incrementally, at different fO 2 , and did not cool significantly (0°C-30°C) prior to its disruption. It remained isotopically heterogenous, but the initial concentration of major elements (SiO 2 , MgO, CaO, Al 2 O 3 , alkali elements) was similar in the different mantle reservoirs.

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“…For some scientists, its diameter was about 200 km (e.g., Wilson et al, 2008). For others, this object was a large planetary embryo with a diameter of at least 690 km Warren, 2012;Barrat et al, 2017), and may have been much larger, possibly the size of Mars (Nabiei et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

Zinc isotopic variations in ureilites

Brugier

Barrat

Guéguen

et al. 2019

Geochimica et Cosmochimica Acta

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Carbon isotopic variation in ureilites: Evidence for an early, volatile-rich Inner Solar System

Cited by 27 publications

References 43 publications

Metamorphism of four desert ureilites and luminescence spectroscopy of defects in ureilitic diamonds

Metamorphism of four desert ureilites and luminescence spectroscopy of defects in ureilitic diamonds

Incremental melting in the ureilite parent body: Initial composition, melting temperatures, and melt compositions

Zinc isotopic variations in ureilites

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