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The inclusion of rotationally-induced mixing in stellar evolution can alterthe structure and composition of presupernova stars. We survey the effects ofprogenitor rotation on nucleosynthetic yields in Population III and IIsupernovae using the new adaptive mesh refinement (AMR) code CASTRO. We examinespherical explosions in 15, 25 and 40 solar mass stars at Z = 0 and 10^-4 solarmetallicity with three explosion energies and two rotation rates. Rotation inthe Z = 0 models resulted in primary nitrogen production and a strongerhydrogen burning shell which led all models to die as red supergiants. On theother hand, the Z=10^-4 solar metallicity models that included rotation endedtheir lives as compact blue stars. Because of their extended structure, thehydrodynamics favors more mixing and less fallback in the metal free stars thanthe Z = 10^-4 models. As expected, higher energy explosions produce moreenrichment and less fallback than do lower energy explosions, and less massivestars produce more enrichment and leave behind smaller remnants than do moremassive stars. We compare our nucleosynthetic yields to the chemical abundancesin the three most iron-poor stars yet found and reproduce the abundance patternof one, HE 0557-4840, with a zero metallicity 15 solar mass, 2.4 x 10^51 ergsupernova. A Salpeter IMF averaged integration of our yields for Z=0 modelswith explosion energies of 2.4x10^51 ergs or less is in good agreement with theabundances observed in larger samples of extremely metal-poor stars, provided15 solar mass stars are included. Since the abundance patterns of extremelymetal-poor stars likely arise from a representative sample of progenitors, ouryields suggest that low-mass supernovae contributed the bulk of the metals tothe early universe.

The Nucleosynthetic Imprint of 15-40 Solar Mass Primordial Supernovae on Metal-Poor Stars