A small fraction of the olivines in CI and CM chondrites contain solar flare tracks. There are no major compositional differences between the irradiated and nonirradiated olivines, suggesting that they form a single population. Solar flare irradiated grain aggregates and chondrules also occur in CM chondrites. The grain aggregates were irradiated as entities, indicating that they formed prior to solar flare irradiation. Angular distribution data for tracks in irradiated olivine grains suggest a single stage exposure to solar flare radiation in most cases. The combined solar flare track data for olivine grains, grain aggregates, and chondrules require that their irradiation took place with variable shielding and are compatible with the model of Goswami and Lal <1979> in which irradiation took place in the near-surface regions of bodies up to a meter in size. However, they also require partial disaggregation and mixing of these small bodies before or during agglomeration to form larger (>km) objects. Irradiation, fragmentation, and redistribution of CI and CM components in their parent body regoliths was probably minimal.