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The evolution of primordial collapsing clouds and formation ofproto-Population III stars are investigated using three-dimensional ideal MHDsimulation. We calculated the evolution of magnetized primordial clouds fromthe prestellar stage until the epoch after the proto-Population III starformation, spatially resolving both parsec-scale clouds and sub-AU scaleprotostars. The formation process of proto-population III star is characterizedby the ratio of rotational to magnetic energy of the parent cloud. When therotational energy is larger than the magnetic energy, fragmentation occurs inthe collapsing primordial cloud before the proto-Population III star formationand binary or multiple system appears. Instead, when the magnetic energy islarger than the rotational energy, strong jet with >100km s^-1 is driven bycircumstellar disk around the proto-population III star without fragmentation.Thus, even in the early universe, the magnetic field plays an important role inthe star formation process.

Population III Star Formation in Magnetized Primordial Clouds