Radioactive nuclei in the early Solar System: analysis of the 15 isotopes produced by core-collapse supernovae

Abstract: 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: $<sup>{26}$Al, $<sup>{36}$Cl, $<sup>{41}$Ca, $<sup>{53}$Mn, $<sup>{60}$Fe, $<sup>{92}$Nb, $<sup>{97}$Tc, $<sup>{98}$Tc, $<sup>{107}$Pd, $<sup>{126}$Sn, $<sup>{129}$I, $<sup>{135}$Cs, $<sup>{146}$Sm, $<sup>{182}$Hf, and $<sup>{205}$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$<em>{\odot}$, explosion energies between 3.4$\times$10$<sup>{50}$ and 1.8$\times$10$<sup>{52}$ ergs and compact remnant masses between 1.5M$</em>{\odot}$and 4.89M$<em>{\odot}$. 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 $<sup>{92}$Nb and $<sup>{97}$Tc, are the most affected by the remnant mass, $<sup>{92}$Nb varying by five orders of magnitude. Isotopes synthesised primarily in explosive C-burning and explosive He-burning, such as $<sup>{60}$Fe, are most affected by explosion energies. $<sup>{60}$Fe increases by two orders of magnitude from the lowest to the highest explosion energy in the 15M$</em>{\odot}$model. The final yield of each examined SLR is used to compare to literature models.