  The origins of carbonaceous asteroids in the asteroid belt is not fully
understood. The leading hypothesis is that they were not born at their current
location but instead implanted into the asteroid belt early in the Solar System
history. We investigate how the migration and growth of Jupiter and Saturn in
their natal disk impact nearby planetesimals and subsequent planetesimal
implantation into the asteroid belt. We account for the effects of surface
ablation of planetesimals caused by thermal and frictional heating between the
gas-disk medium and planetesimal surface, when planetesimals travel through the
gas disk. We have performed simulations considering planetesimals of different
compositions as water-ice rich planetesimals, water-ice poor planetesimals,
organic-rich planetesimals, and fayalite-rich planetesimals. Our findings
indicate that, regardless of the migration history of the giant planets,
water-ice rich, organic-rich, and fayalite-rich planetesimals implanted into
the asteroid belt generally experience surface ablation during implantation in
the asteroid belt, shrinking in size. Planetesimals with enstatite-like
compositions were inconsequential to surface ablation, preserving their
original sizes. By assuming an initial planetesimal size-frequency
distribution, our results show that -- under the effects of surface ablation --
the planetesimal population implanted into the asteroid belt shows a SFD slope
slightly steeper than that of the initial one. This holds true for all
migration histories of the giant planets considered in this work, but for the
Grand-Tack model where the SFD slope remains broadly unchanged. Altogether, our
results suggest that the largest C-type asteroids in the asteroid belt may have
been born bigger. High-degree surface ablation during implantation into the
asteroid belt may have even exposed the cores of early differentiated C-type
planetesimals.
