International Summer Institute for Modeling in Astrophysics

We present simulations of the collapse of a massive rotating protostellar core assuming conditions characteristic of Population III star formation. Starting with an initially weak magnetic field, we find that the combined action of compression and dynamo processes amplify the field to nearly equipartition levels. At late times, we find the magnetic field is able to buoyantly rise above and below the protostellar disk, producing a large-scale magnetic field.