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The origin of supermassive black holes (with $\gtrsim\!10^9\,M_{\odot}$) inthe early universe (redshift $z \sim 7$) remains poorly understood.Gravitational collapse of a massive primordial gas cloud is a promising initialprocess, but theoretical studies have difficulty growing the black hole fastenough. We focus on the magnetic effects on star formation that occurs in anatomic-cooling gas cloud. Using a set of three-dimensional magnetohydrodynamic(MHD) simulations, we investigate the star formation process in the magnetizedatomic-cooling gas cloud with different initial magnetic field strengths. Oursimulations show that the primordial magnetic seed field can be quicklyamplified during the early accretion phase after the first protostar formation.The strong magnetic field efficiently extracts angular momentum from accretinggas and increases the accretion rate, which results in the high fragmentationrate in the gravitationally unstable disk region. On the other hand, thecoalescence rate of fragments is also enhanced by the angular momentum transferdue to the magnetic effects. Almost all the fragments coalesce to the primarystar, so the mass growth rate of the massive star increases due to the magneticeffects. We conclude that the magnetic effects support the direct collapsescenario of supermassive star formation.

Supermassive Star Formation in Magnetized Atomic-Cooling Gas Clouds: Enhanced Accretion, Intermittent Fragmentation, and Continuous Mergers