Formation of Carbonaceous Chondrites in a Jupiter-Induced Pressure Bump

Carbonaceous chondrites (CC) are some of the most primitive meteorites in our Solar System, and their parent bodies likely formed a few Myr after the formation of the Solar System began. CC contain three major components: refractory inclusions, chondrules, and CI chondrite-like matrix. Isotopic studies reveal that the relative abundances of these components correlate with the formation time of their parent bodies. It has been proposed that variations in these abundances reflect the trapping of refractory inclusions and chondrule precursors within pressure maxima in the protoplanetary disk, likely associated with the gap created during Jupiter’s formation.

In this talk, we present Monte Carlo simulations of dust evolution to test whether CC parent bodies could have formed in the outer regions of a Jupiter-induced gap. Our model tracks the transport and collisional evolution of refractory inclusions, chondrules, and matrix-like grains during the late stages of disk evolution. We demonstrate that the observed correlation between the component abundances and the accretion time of the parent body is consistently reproduced if CC formed in a common region over an extended period.