  A model is proposed in which the light r-process element enrichment in
metal-poor stars is explained via enrichment from a truncated r-process, or
"tr-process." The truncation of the r-process from a generic core-collapse
event followed by a collapse into an accretion-induced black hole is examined
in the framework of a galactic chemical evolution model. The constraints on
this 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 to
the 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 with
turbulent ejection in core collapse supernovae. Adaptations of this model are
evaluated to account for the scatter in isotopic observables. This is done by
assuming mixing in ejecta in a supernova event.
