论文标题
人口III星形成中的原始磁场：一项磁化分辨率研究
Primordial magnetic fields in Population III star formation: a magnetised resolution study
论文作者
论文摘要
由于原始气体的破碎，人口III星形成了组。尽管已显示均匀的磁场在当今的恒星形成中支持了反对碎片，但尚不清楚现实的k^3/2原始场是否具有相同的效果。当中央密度达到10-13 g cm-3时，我们绕过与模拟湍流发电机相关的问题。我们测试了从10-10-10-8 g CM-3的一系列水槽颗粒产生密度。在测试的范围内，该场没有抑制气体的碎片化，因此无法阻止碎裂程度随着分辨率的增加而增加。在所有种子场和分辨率上，磁场不影响水槽颗粒中的水槽颗粒数量和总质量。除了在模拟框的最高密度区域外，磁压力仍然是气压的优势，在该框的最高密度区域中，它变得等于但从未超过气压。我们的结果表明，将磁场纳入流行III星形成的数值模拟中并不重要。
Population III stars form in groups due to the fragmentation of primordial gas. While uniform magnetic fields have been shown to support against fragmentation in present day star formation, it is unclear whether realistic k^3/2 primordial fields can have the same effect. We bypass the issues associated with simulating the turbulent dynamo by introducing a saturated magnetic field at equipartition with the velocity field when the central densities reaches 10-13 g cm-3. We test a range of sink particle creation densities from 10-10-10-8 g cm-3. Within the range tested, the fields did not suppress fragmentation of the gas and hence could not prevent the degree of fragmentation from increasing with increased resolution. The number of sink particles formed and total mass in sink particles was unaffected by the magnetic field across all seed fields and resolutions. The magnetic pressure remained sub-dominant to the gas pressure except in the highest density regions of the simulation box, where it became equal to but never exceeded gas pressure. Our results suggest that the inclusion of magnetic fields in numerical simulations of Pop III star formation is largely unimportant.
