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We investigate the dissipation of magnetic flux in primordial star-formingclouds throughout their collapse including the run-away collapse phase as wellas the accretion phase. We solve the energy equation and the non-equilibriumchemical reactions in the collapsing gas, in order to obtain the radialdistribution of the ionized fraction during the collapse. As a result, we findthe ionized fraction is high enough for the magnetic field to couple with thegas throughout the evolution of the cloud. This result suggests that the jetformation from protostars as well as the activation of magneto-rotationalinstability in the accretion disk are enabled in the presence of thecosmological seed magnetic flux proposed by Langer et al.(2003).

Dissipation of Magnetic Flux in Primordial Star Formation: From Run-away Phase to Mass Accretion Phase