In the nascent solar system the decay heat from short-lived radioisotopes (SLRs), in particular the externally
injected aluminum-26, determined thermal and geodynamical transformation of planetesimals and embryos and the
degree of volatile loss by outgassing. Hence, the degree of heating in early planetary bodies is intrinsically
linked to the star formation environment of the solar system. Constraining the injection channel of the solar
system and the statistical distribution of SLRs among planetary systems is thus crucial to compare the planet
formation pathway of the solar system to its stellar siblings. In this talk, I will discuss the relevance of
intra-cluster enrichment mechanisms for the injection of SLRs in young star-forming regions and show how the
pollution of planet-forming systems from supernova ejecta can distribute SLRs across small to large clusters
(100-10,000 stars). Depending on the cluster morphology the enrichment levels can vary considerably, allowing
for a large fraction of enriched systems to exhibit excess abundances compared to the solar system. The
supernova pollution mechanism can thus seed a variety of initial abundance levels and resulting radiogenic
heating rates in planetary precursors. Finally, with emphasis on solar system-like SLR levels, I will
demonstrate how these variations affected the thermomechanical evolution of planetesimals in our solar system
and beyond.
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