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A model is proposed in which the light r-process element enrichment inmetal-poor stars is explained via enrichment from a truncated r-process, or"tr-process." The truncation of the r-process from a generic core-collapseevent followed by a collapse into an accretion-induced black hole is examinedin the framework of a galactic chemical evolution model. The constraints onthis model imposed by observations of extremely metal-poor stars are explained,and the upper limits in the [Sr/Ba] distributions are found to be related tothe nuclear equation of state in a collapse scenario. The scatter in [Sr/Ba]and [Sr/Eu] as a function of metallicity has been found to be consistent withturbulent ejection in core collapse supernovae. Adaptations of this model areevaluated to account for the scatter in isotopic observables. This is done byassuming mixing in ejecta in a supernova event.

Dependence of the Sr-to-Ba and Sr-to-Eu Ratio on the Nuclear Equation of State in Metal Poor Halo Stars