论文标题
人口III恒星系统的动态演变和由此产生的二进制统计数据
Dynamical evolution of Population III stellar systems and the resulting binary statistics
论文作者
论文摘要
我们使用N体模拟来研究种群III（POP III）恒星系统的动力学演变和由此产生的二进制统计数据。我们基于小规模的流体动力模拟和POP III星形成期间磁盘演化的无尺度性质，为POP III星团的初始条件设计了一个物理动机的框架。我们的新方法使我们能够探索二进制统计数据对初始条件的依赖性，并对POP III Protostar Systems的简单外推，对POP III X射线二进制文件（XRB）和二进制黑洞（BBH）合并的信号得出了更强的预测。我们发现，二进制特性对初始群集大小和二元分离的分布高度敏感，而初始质量函数的效果相对较小。我们的模拟预测二进制文件的较差，因此，POP III XRBS的形成和效率显着降低（$ \ sim 10-10^{4} $），这比以前的研究发现，这意味着Pop III XRB对Cosmic X-ray的贡献对宇宙X-ray的贡献是对宇宙X射线的贡献，它们对他们的回馈效果是无效的。我们将POP III BBH合并的效率估计为$ \ sim 10^{ - 5} -10^{ - 4} \ \ \ \ \ \ \ \ \ \ \ \ \ rm m _ {\ odot}^{ - 1} $，为周围的星星或紧密的binartions互动而在周围的星星上进行3型硬化，以与bbhs contericals inspurations in spurate bbhs bbhs bbhs。所有仿真数据，包括POP III二进制文件和多个系统的目录，都可以公开使用。
We use N-body simulations to study the dynamical evolution of Population III (Pop III) stellar systems and the resulting binary statistics. We design a physically-motivated framework for the initial conditions of Pop III star clusters, based on small-scale hydrodynamic simulations and the scale-free nature of disk evolution during Pop III star formation. Our novel approach enables us to explore the dependence of binary statistics on initial conditions and arrive at more robust predictions for the signals of Pop III X-ray binaries (XRBs) and binary black hole (BBH) mergers, compared to simple extrapolations of Pop III protostar systems. We find that binary properties are highly sensitive to the initial cluster size and distribution of binary separation, while the effect of initial mass function is relatively minor. Our simulations predict less close binaries, and thus, significantly lower efficiencies (by a factor of $\sim 10-10^{4}$) for the formation and accretion of Pop III XRBs, than found in previous studies, implying that the contribution of Pop III XRBs to the cosmic X-ray background is negligible and their feedback effects are unimportant. We estimate the efficiency of Pop III BBH mergers as $\sim 10^{-5}-10^{-4}\ \rm M_{\odot}^{-1}$, for which 3-body hardening by surrounding stars in dense star clusters or close binary interactions is required to facilitate in-spirals of BBHs. All simulation data, including catalogs of Pop III binaries and multiple systems, are publicly available.
