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Abstract

Carbonaceous chondrites are some of the most primitive meteorites in our Solar System. Comprising refractory inclusions, chondrules, and CI chondrite-like matrix, these meteorites originate from planetesimals that accreted a few Myr after the Solar System formation started. Recent research by Hellmann et al. (2023) established a fundamental link between the abundances of chondrules and Calcium-Aluminum-rich Inclusions (CAIs), highlighting their interdependence in meteorite composition. Furthermore, their findings suggested a direct correlation between the abundance of matrix dust within carbonaceous chondrites and the accretion time of their parent bodies. They proposed that variations in these abundances reflect the entrapment of CAIs and chondrule precursors within pressure maxima in the protoplanetary disk, likely associated with the gap opened during the formation of Jupiter. <P />Motivated by these findings, we employ Monte Carlo simulations of dust evolution to explore the plausibility of carbonaceous chondrite parent bodies formation in the outer regions of Jupiter-induced gap. Our investigation includes various collision models between refractory and matrix-like materials. We aim to constrain current models of Solar System formation, as well as the intricate interactions between different constituents of carbonaceous chondrites and their incorporation into planetesimals. Our results could provide valuable benchmarks for future laboratory experiments to elucidate how different materials can stick, bounce, or fragment during collisions in protoplanetary disks.