Abstract
Recent data compilations of abundances of Strontium and Barium in Extremely Metal Poor Stars show that large fluctuations exist in the ratio of the abundances of those elements. Two models exist for explaining those fluctuations, as well as the apparent truncation of data for those elements for stars having metallicity of [Fe/H] < −3.5. We study the factors that place upper limits on the logarithmic ratio [Sr/Ba] in the two models. A model has been developed in which the collapse of type II supernovae may produce a pronounced [Sr/Ba] enhancement in single-site r-process enriched stars. This model is consistent with galactic chemical constraints of light-element enrichment in metal-poor stars.
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