Oxygen isotopic evidence for accretion of Earth’s water before a high-energy Moon-forming giant impact

Greenwood, Richard C.; Barrat, Jean‐Alix; Miller, Martin F.; Anand, M.; Dauphas, N.; Franchi, I. A.; Sillard, Patrick; Starkey, N. A.

doi:10.1126/sciadv.aao5928

Cited by 89 publications

(78 citation statements)

References 54 publications

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“…If the steam and CO 2 atmosphere cooled sufficiently for MO crystallization to occur by the time of the Late Veneer (also referred to as "Late Accretion") then even if Venus lost most/all of its primordial H 2 O through escape processes (Gillmann et al, 2009;Hamano et al, 2013;Lichtenegger et al, 2016) there may have been a second chance to obtain a surface ocean, albeit a shallow one. Recent work by Greenwood et al (2018) implies that Earth may have received as much as 30% of its H 2 O inventory in post-accretion impact delivery, consistent with research that shows that the entire H 2 O budget cannot come from the late veneer (Morbidelli & Wood, 2015). Halliday (2013) concludes that if veneers were common they should be proportional to planetary mass, and hence Venus would have received a percentage of late veneer H 2 O similar to that of Earth.…”

Section: Venus' Early Evolution and Evidence For Watersupporting

confidence: 53%

Venusian Habitable Climate Scenarios: Modeling Venus through time and applications to slowly rotating Venus-Like Exoplanets

Way

Genio

2019

Preprint

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Section: Venus' Early Evolution and Evidence For Watersupporting

confidence: 53%

Venusian Habitable Climate Scenarios: Modeling Venus through time and applications to slowly rotating Venus-Like Exoplanets

Way

Genio

2019

Preprint

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“…The regression equation is expressed as δ' 17 O WST = (0.528 ± 0.002) × δ' 18 O WST – (0.057 ± 0.034). The slope of 0.528 is in good agreement with those from other studies on terrestrial rocks and minerals . The Δ 17 O values are calculated from δ' 18 O WST and δ' 17 O WST values and by assuming that Δ 17 O value of UWG2 garnet ( n = 24) is zero, where λ = 0.528 and γ = −0.065.…”

Section: Methodssupporting

confidence: 85%

“…First, we defined the fractionation line for silicate materials from the regression of the δ' 17 O WST and δ' 18 O WST values in this study (Figure S1, supporting information). The regression equation is expressed as δ' 17 O WST = (0.528 ± 0.002) × δ' 18 O WST -(0.057 ± 0.034).The slope of 0.528 is in good agreement with those from other studies on terrestrial rocks and minerals [19][20][21][22][23]. The Δ17 O values are calculated from δ' 18 O WST and δ' 17 O WST values and by assuming that Δ 17 O value of UWG2 garnet (n = 24) is zero, where λ = 0.528 and γ = −0.065.…”

supporting

confidence: 84%

“…However, this approach can be used only for relative comparison of the samples in oxygen isotope analysis because we cannot assure that the oxygen isotope ratios of UWG2 garnet plot exactly on the fractionation line on the VSMOW scale. Furthermore, the slope of the fractionation line assigned by a measurement of terrestrial samples displays little difference among the sample collections …”

Section: Methodsmentioning

confidence: 99%

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An automated laser fluorination technique for high‐precision analysis of three oxygen isotopes in silicates

Kim

Kusakabe

Park

et al. 2019

Rapid Comm Mass Spectrometry

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Rationale The three oxygen isotopes in terrestrial/extraterrestrial silicates can provide geochemical and cosmochemical information about their origin and secondary processes that result from isotopic exchange. A laser fluorination technique has been widely used to extract oxygen from silicates for δ17O and δ18O measurements by isotope ratio mass spectrometry. Continued improvement of the techniques is still important for high‐precision measurement of oxygen‐isotopic ratios. Methods We adopted an automated lasing technique to obtain reproducible fluorination of silicates using a CO2 laser‐BrF5 fluorination system connected online to an isotope ratio mass spectrometer. The automated lasing technique enables us to perform high‐precision analysis of the three oxygen isotopes of typical reference materials (e.g., UWG2 garnet, NBS28 quartz and San Carlos olivine) and in‐house references (mid‐ocean ridge basalt glass and obsidian). The technique uses a built‐in application of laser control with which the laser power can be varied in a programmed manner with a defocused beam which is in a fixed position. Results The oxygen isotope ratios of some international reference materials analyzed by the manual lasing technique were found to be isotopically lighter with wider variations in δ18O values, whereas those measured by the automated lasing technique gave better reproducibility (less than 0.2‰, 2SD). The Δ17O values, an excess of the δ17O value relative to the fractionation line, also showed high reproducibility (±0.02‰, 2SD). Conclusions The system described herein provides high‐precision δ17O and δ18O measurements of silicate materials. The use of the automated lasing technique followed by careful and controlled purification procedures is preferred to achieve satisfactory isotopic ratio results.

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“…In addition to the Earth, materials from other known planetary bodies have been also analysed for their 146 Sm-142 Nd systematics, including samples from the Moon (returned from Apollo and Luna missions and meteorites), meteorites from Mars, Vesta, and other unknown planetary bodies (e.g., angrites and mesosiderites) (e.g., Stewart et al 1994;Foley et al 2005;Boyet et al 2010;Sanborn et al 2015). The Moon has mass-dependent and mass-independent isotope compositions for many elements (e.g., O, Cr, Ti, Ca, Zr) that are identical within analytical precision or nearly indistinguishable from the Earth within a few tens of parts per million (e.g., Wiechert et al 2001;Spicuzza et al 2007;Hallis et al 2010;Young et al 2016;Greenwood et al 2018) (Fig. 3).…”

Section: Constraints On Planetary Building Blocks From Radiogenic Isomentioning

confidence: 99%

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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Oxygen isotopic evidence for accretion of Earth’s water before a high-energy Moon-forming giant impact

Abstract: We show that the bulk of Earth’s water was delivered before the high-energy collision that led to the formation of the Moon.

Cited by 89 publications

References 54 publications

Venusian Habitable Climate Scenarios: Modeling Venus through time and applications to slowly rotating Venus-Like Exoplanets

Venusian Habitable Climate Scenarios: Modeling Venus through time and applications to slowly rotating Venus-Like Exoplanets

An automated laser fluorination technique for high‐precision analysis of three oxygen isotopes in silicates

Accretion of the Earth—Missing Components?

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