Results from our orbital instability model for different model assumptions. Mass, M, as a function of radius, R, of the simulated planets surviving an orbital instability for the different model assumptions described in Section 2.3.1. The final planets are deemed metal-rich remnants (colored symbols) and non-metal-rich remnants (gray symbols) based on the high-density threshold of Equation (3). The black data points correspond to the observed high-density exoplanets listed in Table 1, with one standard deviation uncertainty bars; planet Mercury is plotted for comparison. The side plots are the Kernel Density Estimates (KDEs) of the radius (top) and mass (left) of the observed high-density planets (black curve) and the simulated metal-rich giant-impact remnants (colored curves). The model KDEs are weighted according to the probability of detection of the simulated metal-rich worlds by transit surveys, to mimic observational bias typical of exoplanetary surveys (Section 2.4).