论文标题
恒星质量原始黑洞对第一星形成的影响
Effects of stellar-mass primordial black holes on first star formation
论文作者
论文摘要
我们使用宇宙学水动力缩放模拟和半分析模型来研究原始黑洞（PBHS）对第一星形成的影响。我们的模型是自sonsect的，结合了两种竞争效果：PBHS和BH积聚反馈引起的初始（等离子）扰动。专注于质量$ \ sim 30 \ rm m _ {\ odot} $的PBH，我们发现PBHS不会更改分子冷静的minihaloes中第一星级形成的标准图片，因为在Parsec中模拟的恒星形成气体云非常相似，而Parsec非常相似。 $ f _ {\ rm pbh} \ sim 10^{ - 4} -0.1暗物质。当中央气体密度达到$ 10^{5} \ rm cm^{ - 3} $时，$ \ sim 2-10 \ \ rm Myr $的动态摩擦时间尺寸，PBHS也不可能将星形磁盘陷入恒星盘并影响Protostars的进化，尽管它们可能会与Protostars互动，但它们也不可能与主要的阶段相互作用。在较大的尺度下，PBH倾向于将恒星形成转移到更大的光环，并加速结构形成。后一种效应在较高的初始过重的地区更强。对于$ f _ {\ rm pbh} \ sim 10^{ - 4} -0.01 $（通过观察限制允许），在$ \ sim2 $ youns $ \ sim2 $ in $ z \ sieldsim 30 $中，主持人口III星的光环的质量分数与$ \ rmmmmmmmmmmm-rmmmm-rmmmm-rmmm-rmmm-rmmm-rmmmmss相似（ $ z \ gtrsim 10 $的宇宙星形成历史很小。我们还发现，原子冷却光环中PBH积聚的Lyman-Werner光子可能有助于形成直接偏转BHS。
We use cosmological hydrodynamic zoom-in simulations and semi-analytical models to study the effects of primordial black holes (PBHs) on first star formation. Our models self-consistently combine two competing effects: initial (isocurvature) perturbations induced by PBHs and BH accretion feedback. Focusing on PBHs with masses $\sim 30\ \rm M_{\odot}$, we find that the standard picture of first star formation in molecular-cooling minihaloes is not changed by PBHs, as the simulated star-forming gas clouds in the central parsec are very similar to those in the $\rm ΛCDM$ case when PBHs make up $f_{\rm PBH}\sim 10^{-4}-0.1$ of dark matter. With a dynamical friction timescale of $\sim 2-10\ \rm Myr$ when the central gas density reaches $10^{5}\ \rm cm^{-3}$, it is also unlikely that PBHs can sink into star-forming discs and affect the evolution of protostars, although they may interact with the stars during the main-sequence stage. At larger scales, PBHs tend to shift star formation to more massive haloes, and accelerate structure formation. The latter effect is stronger in regions with higher initial overdensities. For $f_{\rm PBH}\sim 10^{-4}-0.01$ (allowed by observational constraints), the collapsed mass fraction of haloes hosting Population III stars is similar (within a factor of $\sim2$ at $z\lesssim 30$) to that in $\rm ΛCDM$, implying that the impact of stellar-mass PBHs on the cosmic star formation history at $z\gtrsim 10$ is small. We also find that the Lyman-Werner photons from PBH accretion in atomic-cooling haloes may facilitate the formation of direct-collapse BHs.
