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We review models of chondrite component transport in the gaseousprotoplanetary disk. Refractory inclusions were likely transported by turbulentdiffusion and possible early disk expansion, and required low turbulence fortheir subsequent preservation in the disk, possibly in a dead zone. Chondruleswere produced locally but did not necessarily accrete shortly after formation.Water may have been enhanced in the inner disk because of inward drift ofsolids from further out, but likely not by more than a factor of a few.Incomplete condensation in chondrites may be due to slow reaction kineticsduring temperature decrease. While carbonaceous chondrite compositions might bereproduced in a ``two-component'' picture (Anders 1964), such components wouldnot correspond to simple petrographic constituents, although part of therefractory element fractionations in chondrites may be due to the inward driftof refractory inclusions. Overall, considerations of chondrite componenttransport alone favor an earlier formation for carbonaceous chondrites relativeto their noncarbonaceous counterparts, but independent objections have yet tobe resolved.

Transport of solids in protoplanetary disks: Comparing meteorites and astrophysical models