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The ubiquity of turbulence in the primordial minihalos has b een shown from cosmological hydrodynamical simulations of primordial star formation. This h as strong implications on the subsequent evolution, in particular on the generation of magneti c fields via small-scale dynamo action. Using high-resolution numerical simulations, we show that in the presence of turbulence, initial weak seed magnetic fields are exponentially amplified by the s mall-scale dynamo during the formation of the first stars. The field amplification due to the dyn amo is shown to provide additional amplification over what is expected from pure gravitational compression of the field lines. We find that the presence of the small-scale dynamo can only be id entified in numerical simulations where the turbulent motions in the central collapsing core a re resolved by at least 32 grid cells. We conclude that strong magnetic fields are generated during the birth of the first stars in the universe and discuss implications for cosmic evolution.

The generation of strong magnetic fields during the formation of the first stars