  Short-lived radioactive isotopes (SLRs) with half-lives between 0.1 to 100
Myr can be used to probe the origin of the Solar System. In this work, we
examine the core-collapse supernovae production of the 15 SLRs produced:
$^{26}$Al, $^{36}$Cl, $^{41}$Ca, $^{53}$Mn, $^{60}$Fe, $^{92}$Nb, $^{97}$Tc,
$^{98}$Tc, $^{107}$Pd, $^{126}$Sn, $^{129}$I, $^{135}$Cs, $^{146}$Sm,
$^{182}$Hf, and $^{205}$Pb. We probe the impact of the uncertainties of the
core-collapse explosion mechanism by examining a collection of 62 core-collapse
models with initial masses of 15, 20, and 25M$_{\odot}$, explosion energies
between 3.4$\times$10$^{50}$ and 1.8$\times$10$^{52}$ ergs and compact remnant
masses between 1.5M$_{\odot}$and 4.89M$_{\odot}$. We identify the impact of
both explosion energy and remnant mass on the final yields of the SLRs.
Isotopes produced within the innermost regions of the star, such as $^{92}$Nb
and $^{97}$Tc, are the most affected by the remnant mass, $^{92}$Nb varying by
five orders of magnitude. Isotopes synthesised primarily in explosive C-burning
and explosive He-burning, such as $^{60}$Fe, are most affected by explosion
energies. $^{60}$Fe increases by two orders of magnitude from the lowest to the
highest explosion energy in the 15M$_{\odot}$model. The final yield of each
examined SLR is used to compare to literature models.
