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

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.