  Accretion processes in protoplanetary disks produce a diversity of small
bodies that played a crucial role in multiple reshuffling events throughout the
solar system and in both early and late accretion of planets. Application of
thermo-chronometers to meteorites provides precise dating of the formation age
of mineralogical components. Nucleosynthetic anomalies indicating a dichotomy
between NC and C meteorites and precise parent body (PB) chronology can be
combined with thermal evolution models to constrain the timescale of accretion
and dynamical processes in the early solar system. Achondrite PBs are
considered to have accreted early and mostly in the NC region, while late
accretion in the C region produced mostly undifferentiated PBs, such as the CR
chondrite PB that formed as late as 4 Ma after CAIs. However, presence of more
evolved CR-related meteorites suggests also an earlier accretion timing. We
present modeling evidence for a temporally distributed accretion of parent
bodies of CR-related meteorite groups that originate from a C reservoir and
range from aqueously altered chondrites to partially differentiated primitive
achondrites. The PB formation times derived range from <1 Ma to ~4 Ma after
solar system formation, with ~3.7 Ma, ~1.5-2.75 Ma, <~0.6 Ma, and <~0.7 Ma for
CR, Flensburg, NWA 6704, and NWA 011. This implies that accretion processes in
the C reservoir started as early as in the NC reservoir and produced
differentiated PBs with carbonaceous compositions in addition to
undifferentiated C chondritic PBs. The accretion times correlate inversely with
the degree of the meteorites' alteration, metamorphism, or differentiation.
Accretion times for CI/CM, Ryugu, and Tafassites PBs of ~3.75 Ma, ~1-3 Ma, and
1.1 Ma, respectively, fit well into this correlation in agreement with the
thermal and alteration conditions suggested by the meteorites.
