2025/09/25 by Thomas C. L. Truemam, Truemam, Thomas C. L., Andrés Yagüe López +5 · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astronomical and nuclear sciences #Nuclear physics research studies
paper · pdf · doi:10.48550/arxiv.2509.20956
Several short-lived radionuclides (SLRs) are know to have existed in the early Solar System (ESS). These species, which typically decay with half-lives of the order of a few million years, can be used to probe the timescale of events preceding the birth of the Sun. We investigate the ESS origin of 53Mn, produced by core-collapse (CCSNe) and Type Ia supernovae (SNe Ia), and 60Fe, produced exclusively by CCSNe. We model the evolution of the radioactive-to-stable abundance ratios of these SLRs with a galactic chemical evolution (GCE) framework accounting for different supernova yields, SN Ia delay times, and other galactic features (K). A further set of models are calculated assuming that SN Ia did not contribute any 53Mn to the ESS. The predicted ratios are compared to meteoritic ratios to derive a distribution of solar isolation times that includes uncertainties due to stochastic chemical enrichment and precision of the ESS values. The isolation times are then compared to those of 107Pd and 182Hf calculated in previous work. A self-consistent solution can be found within the current uncertainties, especially when using the GCE setups with K = 1.6 and 2.3, although the maximum likelihood for the \iso60Fe distribution is typically ∼ 4-5 Myr shorter than for \iso53Mn. The predicted \iso60Fe/\iso53Mn ratio, instead, is completely inconsistent with the ESS value; this could be resolved using a larger fraction of faint CCSNe than usually considered in GCE models.