  Despite being all roughly of solar composition, primitive meteorites
(chondrites) present a diversity in their chemical, isotopic and petrographic
properties, and in particular a first-order dichotomy between carbonaceous and
non-carbonaceous chondrites. We investigate here analytically the dynamics of
their components (chondrules, refractory inclusions, metal/sulfide and matrix
grains) in protoplanetary disks prior to their incorporation in chondrite
parent bodies. We find the dynamics of the solids, subject to gas drag, to be
essentially controlled by the "gas-solid decoupling parameter" $S\equiv
\textrm{St}/\alpha$, the ratio of the dimensionless stopping time to the
turbulence parameter. The decoupling of the solid particles relative to the gas
is significant when $S$ exceeds unity. $S$ is expected to increase with time
and heliocentric distance. On the basis of (i) abundance of refractory
inclusions (ii) proportion of matrix (iii) lithophile element abundances and
(iv) oxygen isotopic composition of chondrules, we propose that non-matrix
chondritic components had $S<1$ when carbonaceous chondrites accreted and $S>1$
when the other chondrites accreted. This suggests that accretion of
carbonaceous chondrites predated on average that of the other chondrites and
that refractory inclusions are genetically related to their host carbonaceous
chondrites.
