The evolution of collapsing primordial clouds and the formation of Population III (Pop III) protostars are investigated with three-dimensional ideal MHD simulations. We follow the collapse of parsec-sized primordial clouds down to the formation of protostars on sub-AU scales. Pop III protostar formation is characterized by the ratio of rotational to magnetic energy of the natal cloud. When the rotational energy is larger than the magnetic energy, fragmentation occurs prior to the forination of the protostar, and a binary or multiple system appears. When the magnetic energy is greater than the rotational energy, a strong (＞ 100 km s~(-1)) jet is driven by the circumstellar disk around the protostar. which does not fragment. Thus, even in the early universe, magnetic fields play an important role in the star formation process.
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机译：采用三维理想MHD模拟研究了折叠原始云的演变和群体III（POP III）质子的形成。我们遵循对Parsec大小的原始云的崩溃下来，以形成亚AU尺度的质子。 POP III矩阵形成的特征在于旋转与新云的磁能的比率。当旋转能量大于磁性能量时，在对蛋白质的前导之前发生碎片，并且出现二元或多个系统。当磁能大于旋转能量时，强（> 100km S〜（-1））射流由矩质子周围的周围的外围盘驱动。哪个不片段。因此，即使在早期宇宙中，磁场也在星形成过程中起重要作用。
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