The advent of nontraditional isotopic systems (e.g., Ti, Cr, Mo) revealed the presence of a fundamental isotopic dichotomy between non-carbonaceous (NC) and carbonaceous (CC) meteorites. This dichotomy reflects the formation of their parent bodies in two genetically distinct, contemporaneous, but spatially separated disk reservoirs. The barrier separating the inner (NC) from the outer (CC) reservoir has been attributed to the early formation of Jupiter, a long-lived pressure maximum or evolving ice lines in the disk. As the nature of the NC/CC barrier is debated, so is its permeability, such that current inferences range from a hard barrier with almost no influx of outer solar system material to the inner disk, to a soft barrier with large amounts of outer solar system dust passing through the inner disk towards the Sun. During this seminar, I will present new isotopic measurements of NC chondrules that allows to test the permeability of the NC-CC barrier and how the results can affect our understanding of terrestrial planet formation.