第一颗超大质量恒星的诞生
Rise of the First Super-Massive Stars
摘要：
我们使用高分辨率自适应网格细化模拟来模拟早期宇宙中大质量无金属恒星的形成。分别利用100 J $_{21}$和1000 J $_{21}$的Lyman-Werner（LW）背景，构造了有利于大质量恒星形成的环境。我们发现，只有在更高的LW背景的情况下，超临界吸积率实现超大质量恒星（SMS）的形成是必要的。两种背景均观察到轻度碎片化。在更大质量的晕中（1000 J的$_{21}$背景），恒星之间的剧烈动力学相互作用导致两颗最大质量的恒星最终从晕中被驱逐。在较小的质量晕（100 J $_{21}$背景）合并的恒星发生之前，任何多体相互作用和一个单一的大规模流行III星是留在我们的模拟结束时的中心晕。来自非常巨大的Pop III恒星的反馈在产生一个大的HII区域时是无效的，电离光子在恒星的几千AU内被吸收。在所有情况下，巨大的黑洞种子都是最大质量物体的预期最终命运。大质量的波普III型恒星的种子仍然在中心的质量较小的晕经验稳定的吸积率几乎$10^{-2}$ M $_{\odot}$ /年，如果这些利率继续可能会遇到超级爱丁顿吸积率在崩溃后立即成为一个黑洞。
英文摘要：
We use high resolution adaptive mesh refinement simulations to model the formation of massive metal-free stars in the early Universe. By applying Lyman-Werner (LW) backgrounds of 100 J$_{21}$ and 1000 J$_{21}$ respectively we construct environments conducive to the formation of massive stars. We find that only in the case of the higher LW backgrounds are super-critical accretion rates realised that are necessary for super-massive star (SMS) formation. Mild fragmentation is observed for both backgrounds. Violent dynamical interactions between the stars that form in the more massive halo formed (1000 J$_{21}$ background) results in the eventual expulsion of the two most massive stars from the halo. In the smaller mass halo (100 J$_{21}$ background) mergers of stars occur before any multibody interactions and a single massive Pop III star is left at the centre of the halo at the end of our simulation. Feedback from the very massive Pop III stars is not effective in generating a large HII region with ionising photons absorbed within a few thousand AU of the star. In all cases a massive black hole seed is the expected final fate of the most massive objects. The seed of the massive Pop III star which remained at the centre of the less massive halo experiences steady accretion rates of almost $10^{-2}$ M$_{\odot}$/yr and if these rates continue could potentially experience super-Eddington accretion rates in the immediate aftermath of collapsing into a black hole.
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