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The fundamentally different isotopic compositions of non-carbonaceous (NC)and carbonaceous (CC) meteorites reveal the presence of two distinct reservoirsin the solar protoplanetary disk that were likely separated by Jupiter.However, the extent of material exchange between these reservoirs, and how thisaffected the composition of the inner disk are not known. Here we show that NCmeteorites display broadly correlated isotopic variations for Mo, Ti, Cr, andNi, indicating the addition of isotopically distinct material to the innerdisk. The added material resembles bulk CC meteorites and Ca-Al-rich inclusionsin terms of its enrichment in neutron-rich isotopes, but unlike the lattermaterials is also enriched in s-process nuclides. The comparison of theisotopic composition of NC meteorites with the accretion ages of their parentbodies reveals that the isotopic variations within the inner disk do notreflect a continuous compositional change through the addition of CC dust,indicating an efficient separation of the NC and CC reservoirs and limitedexchange of material between the inner and outer disk. Instead, the isotopicvariations among NC meteorites more likely record a rapidly changingcomposition of the disk during infall from the Sun's parental molecular cloud,where each planetesimal locks the instant composition of the disk when itforms. A corollary of this model is that late-formed planetesimals in the innerdisk predominantly accreted from secondary dust that was produced by collisionsamong pre-existing NC planetesimals.

Isotopic evolution of the inner Solar System inferred from molybdenum isotopes in meteorites