  The current properties of small bodies provide important clues to their
origin and history. However, how much small bodies were processed by past
collisions and to what extent they retain a record of processes that took place
during the formation and early evolution of the Solar System is still poorly
understood. Here we study the degree of collisional heating and compaction by
analysing the large set of previous simulations of small body break-ups by
Jutzi et al. (2019), which used porous targets of 50 - 400 km in diameter and
investigated a large range of impact velocities, angles as well as energies. We
find that the degree of impact processing is generally larger than found in
previous studies which considered smaller objects (e.g. Jutzi et al., 2017;
Schwartz et al., 2018). However, there is a clear dichotomy in terms of impact
processing: the escaping material always experiences stronger heating than the
material bound to the largest remnant. Assuming they originate from the same
parent body, some of the observed differences between the recently visited
asteroids Ryugu and Bennu may be explained by a different location of the
material eventually forming these asteroids in the original parent body. Our
results also provide constraints on the initial size of cometary nuclei.
