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GW170817 has confirmed binary neutron star mergers as one of the sites forrapid neutron capture ($r$) process. However, there are large theoretical andexperimental uncertainties associated with the resulting nucleosynthesiscalculations and additional sites may be needed to explain all the existingobservations. In this regard, abundances of short-lived radioactive isotopes(SLRIs) in the early solar system (ESS), that are synthesized exclusively by$r$-process, can provide independent clues regarding the nature of $r$-processevents. In this work, we study the evolution of $r$-process SLRIs $^{129}$I and$^{247}$Cm as well as the corresponding reference isotopes $^{127}$I and$^{235}$U at the Solar location. We consider up to three different sources thathave distinct $^{129}$I/$^{247}$Cm production ratios corresponding to thevaried $r$-process conditions in different astrophysical scenarios. In contrastto the results found by C\^ot\'e et al. (2021), we find that $^{129}$I and$^{247}$Cm in the ESS do not come entirely from a single major event but getcontributions from at least two more minor contributors. This has a dramaticeffect on the evolution of the $^{129}$I/$^{247}$Cm ratio, such that themeasured ESS value in meteorites may not correspond to that of the "$last$"major $r$-process event. Interestingly, however, we find that the$^{129}$I/$^{247}$Cm ratio, in combination with the observed$^{129}$I/$^{127}$I and $^{247}$Cm/$^{235}$U ratio in the ESS, can stillprovide important constraints on the properties of proposed $r$-process sourcesoperating in the Milky Way.

Constraints on $R$-process Nucleosynthesis from $^{129}$I and $^{247}$Cm in the Early Solar System