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We report the results of the first self-consistent three-dimensional adaptivemesh refinement magnetohydrodynamical simulations of Population III starformation including the Biermann Battery effect. We find that the PopulationIII stars formed including this effect are both qualitatively andquantitatively similar to those from hydrodynamics-only (non-MHD) cosmologicalsimulations. We observe peak magnetic fields of ~10^-9 G in the center of ourstar-forming halo at z ~ 17.55. The magnetic fields created by the BiermannBattery effect are predominantly formed early in the evolution of theprimordial halo at low density and large spatial scales, and then grow throughcompression and by shear flows. The fields seen in this calculation are neverlarge enough to be dynamically important (with beta >= 10^{15} at all times),and should be considered the minimum possible fields in existence duringPopulation III star formation, and may be seed fields for the stellar dynamo orthe magnetorotational instability at higher densities and smaller spatialscales.

The Biermann Battery in Cosmological MHD Simulations of Population III Star Formation