论文标题
触发人口III星形成：h $ _2 $自我屏蔽的效果
Triggered Population III star formation: the effect of H$_2$ self-shielding
论文作者
论文摘要
无金属（种群III）恒星的多种性可能会影响其在宿主暗物质中的反馈效率，从而影响随后的金属富集和向星系形成的过渡。来自大型恒星的辐射反馈可以在密集的自屏云中触发附近的恒星形成。在模型辐射自屏蔽中，必须精确计算H $ _2 $列密度。在这项研究中，我们比较了两个基于密度梯度和牛仔裤长度的局部近似值，并与沿射线的柱密度直接整合。在主要的大恒星形成之后，我们发现直接整合和密度梯度方法都没有次级恒星形成。近似方法将计算时间减少了2倍。牛仔裤长度近似将H $ _2 $列密度高出10倍，从而导致五个数值增强的自固定的自固定，恒星形成的团块。我们得出的结论是，密度梯度近似足够精确地用于较大的体积星系模拟，尽管仍然必须警告说近似无法完全重现直接整合的结果。
The multiplicity of metal-free (Population III) stars may influence their feedback efficiency within their host dark matter halos, affecting subsequent metal enrichment and the transition to galaxy formation. Radiative feedback from massive stars can trigger nearby star formation in dense self-shielded clouds. In model radiation self-shielding, the H$_2$ column density must be accurately computed. In this study, we compare two local approximations based on the density gradient and Jeans length with a direct integration of column density along rays. After the primary massive star forms, we find that no secondary stars form for both the direct integration and density gradient approaches. The approximate method reduces the computation time by a factor of 2. The Jeans length approximation overestimates the H$_2$ column density by a factor of 10, leading to five numerically enhanced self-shielded, star-forming clumps. We conclude that the density gradient approximation is sufficiently accurate for larger volume galaxy simulations, although one must still caution that the approximation cannot fully reproduce the result of direct integration.
