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The Role of Radial Transport in Forming Minor Bodies of the Outer Solar System

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Abstract

In this paper, we summarize the experimental data on the features of the mineral, chemical, and isotopic compositions of minor bodies of the Solar System—asteroids, Saturn’s satellites, and nuclei of comets of different dynamic types—which suggest that the formation of these bodies was significantly influenced by the mixing of different-genesis matter: presolar and nebular. The latter was formed in the circumsolar gas–dust protoplanetary accretion disk that is also called the nebula. The matter of presolar origin includes amorphous iron–magnesium silicates, refractory organic compounds, volatile organic compounds, amorphous water ice, as well as ices of СО2, NH3, CH3OH, CO, etc. The species of nebular origin are aluminum-, calcium-, and titanium-rich refractory inclusions (known as CAls), microcrystalline magnesium silicates, as well as crystalline water ice, the hydrogen isotopic composition of which is several times lower than that of water ice of the protosolar nebula. The presolar- and nebular-origin matter could be mixed because, in the circumsolar disk at the early stages of its evolution, in addition to the main accretion flux of the gas–dust matter passing through the disk toward the Sun, there was a flux moving in the opposite direction, from the Sun, from the inner hot regions of the circumsolar disk outward to its external regions. There, the nebular matter was mixed with the protosolar matter, which had been precipitating onto the disk from its accretion envelope, mainly onto its edge, during the first million years of its evolution. The currently available package of the experimental data allows us to suppose that it is exactly the mixing of the matter from two regions of the circumsolar disk, within which the P–T conditions significantly differed, that may explain the presence of chemically and isotopically heterogeneous ice–rock bodies in the outer Solar System.

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    V. A. Dorofeeva

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Dorofeeva, V.A. The Role of Radial Transport in Forming Minor Bodies of the Outer Solar System. Sol Syst Res 56, 168–182 (2022). https://doi.org/10.1134/S0038094622020034

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