GENERATION OF MAGNETIC FIELD ON THE ACCRETION DISK AROUND A PROTO-FIRST-STAR

The generation process of a magnetic field around a proto-first-star is studied. Utilizing the recent numerical results of proto-first-star formation based on radiation hydrodynamics simulations, we assess the magnetic field strength generated by the radiative force and the Biermann battery effect. We find that a magnetic field of ~10 super(-9) G is generated on the surface of the accretion disk around the proto-first-star. The field strength on the accretion disk is smaller by two orders of magnitude than the critical value, above which the gravitational fragmentation of the disk is suppressed. Thus, the generated seed magnetic field hardly affect the dynamics of on-site first star formation directly, unless an efficient amplification process is taken into consideration. We also find that the generated magnetic field is continuously blown out from the disk on the outflows to the poles, that are driven by the thermal pressure of photoheated gas. The strength of the diffused magnetic field in low-density regions is ~10 super(-14)-10 super(-13) G at n sub(H) = 10 super(3) cm super(-3), which could play an important role in the next generation star formation, as well as the seeds of the magnetic field in the present-day universe.