  Rocky planets both in and outside of our solar system are observed to have a
range of core-mass fractions (CMFs). Imperfect collisions can preferentially
strip mantle material from a planet, changing its CMF, and are therefore
thought to be the most likely cause of this observed CMF variation. However,
previous work that implements these collisions into N-body simulations of
planet formation has struggled to reliably form high CMF super-Earths. In this
work, we specify our initial conditions and simulation parameters to maximize
the prevalence of high-energy, CMF-changing collisions in order to form planets
with highly diverse CMFs. High-energy collisions have a large $v_{imp}/v_{esc}$
ratio, so we maximize this ratio by starting simulations with high-eccentricity
and inclination disks to increase the difference in their orbital velocities,
maximizing $v_{imp}$. Additionally, we minimize $v_{esc}$ by starting with
small embryos. The final planets undergo more high-energy, debris-producing
collisions, and experience significant CMF change over their formation.
However, we find that a number of processes work together to average out the
CMF of a planet over time, therefore we do not consistently form high-CMF, high
mass planets. We do form high-CMF planets below 0.5 $M_{\oplus}$. Additionally,
we find in these highly eccentric environments, loss of debris mass due to
collisional grinding has a significant effect on final planet masses and CMFs,
resulting in smaller planets and a higher average planet CMF. This work
highlights the importance of improving measurements of high-density planets to
better constrain their CMFs.
