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Chondrules formed by the melting of dust aggregates in the solarprotoplanetary disk and as such provide unique insights into how solid materialwas transported and mixed within the disk. Here we show that chondrules fromenstatite and ordinary chondrites show only small 50Ti variations and scatterclosely around the 50Ti composition of their host chondrites. By contrast,chondrules from carbonaceous chondrites have highly variable 50Ti compositions,which, relative to the terrestrial standard, range from the small 50Ti deficitsmeasured for enstatite and ordinary chondrite chondrules to the large 50Tiexcesses known from Ca-Al-rich inclusions (CAIs). These 50Ti variations can beattributed to the addition of isotopically heterogeneous CAI-like material toenstatite and ordinary chondrite-like chondrule precursors. The new Ti isotopicdata demonstrate that isotopic variations among carbonaceous chondritechondrules do not require formation over a wide range of orbital distances, butcan instead be fully accounted for by the incorporation of isotopicallyanomalous nuggets into chondrule precursors. As such, these data obviate theneed for disk-wide transport of chondrules prior to chondrite parent bodyaccretion and are consistent with formation of chondrules from a givenchondrite group in localized regions of the disk. Lastly, the ubiquitouspresence of 50Ti-enriched material in carbonaceous chondrites, and the lack ofthis material in the non-carbonaceous chondrites support the idea that thesetwo meteorite groups derive from areas of the disk that remained isolated fromeach other through the formation of Jupiter.

Mixing and transport of dust in the early solar nebula as inferred from titanium isotope variations among chondrules