  Compilations of abundances of Strontium and Barium in extremely metal-poor
stars show that an apparent cutoff is observed for [Sr/Ba] at [Fe/H]$<$-3.6 and
large fluctuations for [Fe/H]$>$-3.6 with a clear upper bound depending on
metallicity. We study the factors that place upper limits on the logarithmic
ratio [Sr/Ba]. A model is developed in which the collapses of type II
supernovae are found to reproduce many of the features seen in the data. This
model is consistent with galactic chemical evolution constraints of
light-element enrichment in metal-poor stars. Effects of turbulence in an
explosive site have also been simulated, and are found to be important in
explaining the large scatter observed in the [Sr/Ba] data.
