Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water

By D. Rubie, Seth Andrew Jacobson, A. Morbidelli, D. O'Brien, E. Young, J. de Vries, H. Palme, D. Frost. 2014

389 citations recorded by the source corpus.

Abstract In order to test accretion simulations as well as planetary differentiation scenarios, we have integrated a multistage core–mantle differentiation model with N-body accretion simulations. Impacts between embryos and planetesimals are considered to result in magma ocean formation and episodes of core formation. The core formation model combines rigorous chemical mass balance with metal–silicate element partitioning data and requires that the bulk compositions of all starting embryos and planetesimals are defined as a function of their heliocentric distances of origin. To do this, we assume that non-volatile elements are present in Solar System (CI) relative abundances in all bodies and that oxygen and H2O contents are the main compositional variables. The primary constraint on the combined model is the composition of the Earth’s primitive mantle. In addition, we aim to reproduce the composition of the martian mantle and the mass fractions of the metallic cores of Earth and Mars. The model is refined by least squares minimization with up to five fitting parameters that consist of the metal–silicate equilibration pressure and 1–4 parameters that define the starting compositions of primitive bodies. This integrated model has been applied to six Grand Tack N-body accretion simulations. Investigations of a broad parameter space indicate that: (1) accretion of Earth was heterogeneous, (2) metal–silicate equilibration pressures increase as accretion progresses and are, on average, 60–70% of core–mantle boundary pressures at the time of each impact, and (3) a large fraction (70–100%) of the metal of impactor cores equilibrates with a small fraction of the silicate mantles of proto-planets during each core formation event. Results are highly sensitive to the compositional model for the primitive starting bodies and several accretion/core-formation models can thus be excluded. Acceptable fits to the Earth’s mantle composition are obtained only when bodies that originated close to the Sun, at

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fc3e948bdf5e52f55a78337c9cc6b663e42f22cc

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In Astronomy and Astrophysics

Citations in the corpus

Melting and mixing states of the Earth’s mantle after the Moon-forming impact (2015, background): “However, this model may be too simplistic because it assumes that the core formation occurred by a single stage process, but the Earth’s core must have formed though multiple impacts processes (Wade and Wood, 2005; Rubie et al., 2015).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “Assuming a similar outcome for our simulations, the mechanism presented here appears consistent with the geochemical constraints from Rubie et al. (2015).”
Fossilized condensation lines in the Solar System protoplanetary disk (2015, background): “Furthermore, a significant accretion of oxidized material would have led to an Earth with different chemical properties (Rubie et al., 2015).”