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: ${}^{26}$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.