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Recent high-resolution simulations of early structure formation have shownthat externally enriched halos may form some of the first metal enriched stars.This study utilizes a 1 comoving Mpc$^3$ high-resolution simulation to studythe enrichment process of metal-enriched halos down to $z=9.3$. Our simulationuniquely tracks the metals ejected from Population III stars, and we use thisinformation to identify the origin of metals within metal-enriched halos. Thesehalos show a wide range of metallicities, but we find that the source of metalsfor $\gtrsim$ 50\% of metal-enriched halos is supernova explosions ofPopulation III stars occuring outside their virial radii. The results presentedhere indicate that external enrichment by metal-free stars dominates theenrichment process of halos with virial mass below $10^{6}\,M_\odot$ down to$z=9.3$. Despite the prevalence of external enrichment in low mass halos, PopII stars forming due to external enrichment are rare because of the smallcontribution of low-mass halos to the global star formation rate combined withlow metallicities towards the center of these halos resulting from metal ejectafrom external sources mixing from the outside-in. The enriched stars that doform through this process have absolute metallicities below $10^{-3}\,Z_\odot$.We also find that the fraction of externally enriched halos increases withtime, $\sim 90\%$ of halos that are externally enriched have $M_\mathrm{vir} <10^6\,M_\odot$, and that pair-instability supernovae contribute the most to theenrichment of the IGM as a whole and are thus are the predominant supernovatype contributing to the external enrichment of halos.

External Enrichment of Minihalos by the First Supernovae