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Ruthenium isotopic evidence for an inner Solar System origin of the late veneer

Nature volume 541, pages 525–527 (2017)Cite this article

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Abstract

The excess of highly siderophile elements in the Earth’s mantle is thought to reflect the addition of primitive meteoritic material after core formation ceased1,2,3,4. This ‘late veneer’ either comprises material remaining in the terrestrial planet region after the main stages of the Earth’s accretion5,6, or derives from more distant asteroidal7 or cometary8 sources. Distinguishing between these disparate origins is important because a late veneer consisting of carbonaceous chondrite-like asteroids7 or comets8 could be the principal source of the Earth’s volatiles and water. Until now, however, a ‘genetic’ link between the late veneer and such volatile-rich materials has not been established or ruled out. Such genetic links can be determined using ruthenium (Ru) isotopes, because the Ru in the Earth’s mantle predominantly derives from the late veneer9, and because meteorites exhibit Ru isotope variations arising from the heterogeneous distribution of stellar-derived dust10,11. Although Ru isotopic data and the correlation of Ru and molybdenum (Mo) isotope anomalies in meteorites were previously used to argue that the late veneer derives from the same type of inner Solar System material as do Earth’s main building blocks6, the Ru isotopic composition of carbonaceous chondrites has not been determined sufficiently well to rule them out as a source of the late veneer. Here we show that all chondrites, including carbonaceous chondrites, have Ru isotopic compositions distinct from that of the Earth’s mantle. The Ru isotope anomalies increase from enstatite to ordinary to carbonaceous chondrites, demonstrating that material formed at greater heliocentric distance contains larger Ru isotope anomalies. Therefore, these data refute an outer Solar System origin for the late veneer and imply that the late veneer was not the primary source of volatiles and water on the Earth.

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Figure 1: ϵ100Ru data for chondrites, iron meteorites and terrestrial chromitites.
Figure 2: The magnitude of ϵ100Ru anomalies increases with increasing distance (in astronomical units, au) from the Sun.

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Acknowledgements

We thank the Meteorite Working Group at NASA, A. Bischoff and A. Greshake for providing the meteorite samples for this study, and K. Bermingham and B. O’Driscoll for providing the Shetland chromitite sample. We thank U. Heitmann, T. Kruijer and C. Proksche for their assistance, and A. Brandon, C. Brennecka and D. Papanastassiou for comments on the paper. This work was supported by the Deutsche Forschungsgemeinschaft (SFB-TRR 170, subproject B3-1). This is TRR 170 publication no. 11.

Author information

Authors and Affiliations

  1. Institut für Planetologie, University of Münster, Wilhelm-Klemm-Strasse 10, Münster, 48149, Germany

    Mario Fischer-Gödde & Thorsten Kleine

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  1. Mario Fischer-Gödde
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  2. Thorsten Kleine
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Contributions

M.F.-G. prepared the samples for Ru isotope analyses and conducted the measurements. Both M.F.-G. and T.K. were involved in the interpretation of the data and the writing of the manuscript.

Corresponding authors

Correspondence to Mario Fischer-Gödde or Thorsten Kleine.

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The authors declare no competing financial interests.

Additional information

Reviewer Information Nature thanks A. Brandon and the other anonymous reviewer(s) for their contribution to the peer review of this work.

Extended data figures and tables

Extended Data Figure 1 Ruthenium isotope plots for chondrites and iron meteorites.

a, ϵ100Ru–ϵ96Ru; b, ϵ100Ru–ϵ102Ru. See the source data for Extended Data Fig. 1. Lines represent mixing lines between terrestrial Ru and an s-process component as defined by Ru isotope data for presolar SiC32 (dashed line), calculated s-process yields33 (dotted line) and corresponding calculated residuals for rapid neutron capture process (r-process) of stellar nucleosynthesis (dashed-dotted line). Uncertainties of individual data points reflect the external uncertainty of the method (2 s.d., for samples measured n < 4 times) or 95% confidence intervals (calculated as two-sided Student’s t-values, for samples measured n ≥ 4 times). Uncertainties for group averages of ordinary and enstatite chondrites are 95% confidence intervals, and uncertainties for non-magmatic IAB iron meteorites include propagated errors from secondary neutron-capture correction as given in Extended Data Table 2. Data for other iron meteorites are from ref. 11.

Source data

Extended Data Table 1 Ruthenium isotope data of chondrites and terrestrial chromitites
Full size table
Extended Data Table 2 Measured Ru and Pt isotope data and neutron-capture-corrected ϵiRu values for non-magmatic iron meteorites (group IAB)
Full size table

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Fischer-Gödde, M., Kleine, T. Ruthenium isotopic evidence for an inner Solar System origin of the late veneer. Nature 541, 525–527 (2017). https://doi.org/10.1038/nature21045

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