Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf-W Chronometry of Iron Meteorites

Neumann, W.; Kruijer, T. S.; Breuer, D.; Kleine, T.

doi:10.1002/2017JE005411

Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf-W Chronometry of Iron Meteorites

Journal Article · Thu Feb 01 00:00:00 EST 2018 · Journal of Geophysical Research. Planets

DOI:https://doi.org/10.1002/2017JE005411· OSTI ID:1430986

^[1]; Kruijer, T. S. ^[2]; ^[3]; Kleine, T. ^[4]

Univ. of Munster, Munster (Germany). Inst. fur Planetologie; Deutsches Zentrum fur Luft-und Raumfahrt (DLR), Berlin (Germany)
Univ. of Munster, Munster (Germany). Inst. fur Planetologie; Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States). Nuclear and Chemical Sciences Division
Deutsches Zentrum fur Luft-und Raumfahrt (DLR), Berlin (Germany)
Univ. of Munster, Munster (Germany). Inst. fur Planetologie

Iron meteorites provide some of the most direct insights into the processes and timescales of core formation in planetesimals. Of these, group IVB irons stand out by having one of the youngest ¹⁸²Hf-¹⁸²W model ages for metal segregation (2.9 ± 0.6 Ma after solar system formation), as well as the lowest bulk sulfur content and hence highest liquidus temperature. Here in this paper, using a new model for the internal evolution of the IVB parent body, we show that a single stage of metal-silicate separation cannot account for the complete melting of pure Fe metal at the relatively late time given by the Hf-W model age. Instead, a complex metal-silicate separation scenario is required that includes migration of partial silicate melts, formation of a shallow magma ocean, and core formation in two distinct stages of metal segregation. In the first stage, a protocore formed at ≈1.5 Ma via settling of metal particles in a mantle magma ocean, followed by metal segregation from a shallow magma ocean at ≈5.4 Ma. As these stages of metal segregation occurred at different times, the two metal fractions had different ¹⁸²W compositions. Consequently, the final 182W composition of the IVB core does not correspond to a single differentiation event, but represents the average composition of early- and late-segregated core fractions. Our best fit model indicates an ≈100 km radius for the IVB parent body and provides an accretion age of ≈0.1–0.5 Ma after solar system formation. The computed solidification time is, furthermore, consistent with the Re-Os age for crystallization of the IVB core.

View Accepted Manuscript (DOE)

Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: German Research Foundation (DFG); USDOE

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 1430986

Report Number(s):: LLNL-JRNL--739210

Journal Information:: Journal of Geophysical Research. Planets, Journal Name: Journal of Geophysical Research. Planets Journal Issue: 2 Vol. 123; ISSN 2169-9097

Publisher:: American Geophysical UnionCopyright Statement

Country of Publication:: United States

Language:: English

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