Abstract The models that most successfully reproduce the orbital architecture of the solar system terrestrial planets start from a narrow annulus of material that grows into embryos and then planets. However, it is not clear how this ring model can be made consistent with the chemical structure of the inner solar system, which shows a reduced-to-oxidized gradient from Mercury to Mars and a parallel gradient in the asteroid belt. We propose that there were two primary reservoirs in the early inner solar system: a narrow, refractory-enriched ring inside of 1 au; and a less massive, extended planetesimal disk outside of 1 au, with oxidation states ranging from enstatite chondrites to ordinary chondrites. We show through a suite of N -body simulations that an inwardly sweeping secular resonance, caused by aerodynamic drag and perturbations from a mean-motion resonant Jupiter and Saturn, gathers the outer planetesimal disk into a narrow ring that migrates radially, forms Mars, and contributes oxidized material to proto-Earth. Remaining unaccreted planetesimals can be implanted into the asteroid belt as the parent bodies of aubrites and non-carbonaceous iron meteorites, while the most reduced material is not implanted and thus is unsampled in the meteorite collection. This model explains the oxidation and isotopic gradients within the inner solar system within the context of a low-viscosity, magnetic-wind-driven disk.
Goldberg et al. (Thu,) studied this question.