An updated picture of pre-solar history from short-lived radioactive isotopes and inferences on the birth of the Sun
Benj\'amin So\'os, Thomas C. L. Trueman, Andr\'es Yag\"ue L\'opez, Lorenzo Roberti, Maria Lugaro

TL;DR
This study investigates the origins of short-lived radionuclides in the early Solar System, considering decay and mixing timescales, and finds that some isotopes' abundances can be explained by specific nucleosynthesis scenarios.
Contribution
It introduces a model incorporating decay and mixing timescales to explain the observed radionuclide abundances in the early Solar System.
Findings
ESS abundances of certain isotopes can be explained with decay times of 9-14 Ma.
Some isotopes' abundances cannot be explained by steady-state equilibrium in the ISM.
The model accounts for galactic uncertainties affecting radionuclide predictions.
Abstract
We examine the origin of the short-lived radionuclides (SLRs, defined as having half-lives between 0.1 and 100 Ma) present in the early Solar System (ESS) by investigating how predictions of their abundances in the interstellar medium (ISM) from steady-state equilibrium relate to their ESS values. For this, we take into account the non-negligible time elapsed between the isolation of the pre-solar molecular cloud and the formation of the ESS, during which the SLRs decayed freely. We also consider the alternative scenario in which the pre-solar molecular cloud remained partially mixed with the ISM, with a mixing timescale . We find that the ESS abundances of Pd and Hf produced by \textit{slow} neutron captures (\textit{s}-process), and of Mn and Fe produced by explosive nucleosynthesis, can be consistently explained…
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