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- W4296163795 abstract "The parent cores of iron meteorites belong to the earliest accreted bodies in the solar system. These cores formed in two isotopically distinct reservoirs: noncarbonaceous (NC) type and carbonaceous (CC) type in the inner and outer solar system, respectively. We measured elemental compositions of CC-iron groups and used fractional crystallization modeling to reconstruct the bulk compositions and crystallization processes of their parent asteroidal cores. We found generally lower S and higher P in CC-iron cores than in NC-iron cores and higher HSE (highly siderophile element) abundances in some CC-iron cores than in NC-iron cores. We suggest that the different HSE abundances among the CC-iron cores are related to the spatial distribution of refractory metal nugget-bearing calcium aluminum-rich inclusions (CAIs) in the protoplanetary disk. CAIs may have been transported to the outer solar system and distributed heterogeneously within the first million years of solar system history." @default.
- W4296163795 created "2022-09-18" @default.
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- W4296163795 date "2022-09-16" @default.
- W4296163795 modified "2023-10-14" @default.
- W4296163795 title "Compositions of carbonaceous-type asteroidal cores in the early solar system" @default.
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- W4296163795 doi "https://doi.org/10.1126/sciadv.abo5781" @default.
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