论文标题
庞大的第一星级二进制的诞生
The Birth of a Massive First-Star Binary
论文作者
论文摘要
我们使用新开发的辐射流体动力学代码和自适应网状射线追踪方法研究了大量种群III二进制恒星的形成。我们遵循从宇宙流体动力学模拟获得的典型原始恒星形成云的演变。磁盘碎裂并通过气体积聚形成了几种原始的质体，最终被原恒星的辐射反馈淬灭。我们的代码使我们能够首次考虑与多个原始辐射的电离辐射和解离的反馈，这对于自我谐振的最终质量至关重要。在模拟的最后一步中，我们观察到一个非常宽的（$ \ gtrsim 10^4 \，\ mathrm {au} $）二进制恒星系统，该系统由$ 60 $和$ 70 \，m_ \ odot $ stars组成。其中一颗成员明星还具有两个较小的质量（$ 10 \，m_ \ odot $）伴侣明星，以$ 200 $和$ 800 \，\ mathrm {au} $旋转，构成了一个迷你三个系统。我们的结果表明，在人群III星中，大量二元或多个系统很常见。
We study the formation of massive Population III binary stars using a newly developed radiation hydrodynamics code with the adaptive mesh refinement and adaptive ray-tracing methods. We follow the evolution of a typical primordial star-forming cloud obtained from a cosmological hydrodynamics simulation. Several protostars form as a result of disk fragmentation and grow in mass by the gas accretion, which is finally quenched by the radiation feedback from the protostars. Our code enables us, for the first time, to consider the feedback by both the ionizing and dissociating radiation from the multiple protostars, which is essential for self-consistently determining their final masses. At the final step of the simulation, we observe a very wide ($\gtrsim 10^4\,\mathrm{au}$) binary stellar system consisting of $60$ and $70\,M_\odot$ stars. One of the member stars also has two smaller mass ($10\,M_\odot$) companion stars orbiting at $200$ and $800\,\mathrm{au}$, making up a mini-triplet system. Our results suggest that massive binary or multiple systems are common among Population III stars.
