  Understanding the origin of chondritic components and their accretion
pathways is critical to unravel the magnitude of mass transport in the
protoplanetary disk, the accretionary history of the terrestrial planet region
and, by extension, its prebiotic inventory. Here, we trace the heritage of
pristine components from the relatively unaltered CV chondrite Leoville through
their mass-independent Cr and mass-dependent Zn isotope compositions.
Investigating these chondritic fractions in such detail reveals an onion-shell
structure of chondrules, which is characterized by 54Cr- and 66Zn-poor cores
surrounded by increasingly 54Cr- and 66Zn-rich igneous rims and an outer
coating of fine-grained dust. This is interpreted as a progressive addition of
54Cr- and 66Zn-rich, CI-like material to the accretion region of these
carbonaceous chondrites. Our findings show that the observed Cr isotopic range
in chondrules from more altered CV chondrites is the result of chemical
equilibration between chondrules and matrix during secondary alteration. The
54Cr-poor nature of the cores of Leoville chondrules implies formation in the
inner Solar System and subsequent massive outward chondrule transport past the
Jupiter barrier. At the same time, CI-like dust is transferred inwards. We
propose that the accreting Earth acquired CI-like dust through this mechanism
within the lifetime of the disk. This radial mixing of chondrules and matrix
shows the limited capacity of Jupiter to act as an efficient barrier and
maintain the proposed non-carbonaceous and carbonaceous chondrite dichotomy
over time. Finally, also considering current astrophysical models, we explore
both inner and outer Solar System origins for the CV chondrite parent body.
