论文标题
直接塌陷到超质量黑洞种子的前体：辐射反馈产生的流出
Direct Collapse to Precursors of Supermassive Black Hole Seeds:Radiation-feedback-generated Outflows
论文作者
论文摘要
我们使用高分辨率的缩放宇宙学模拟来模拟在暗物质（DM）光环内直接崩溃期间中央质量积累周围触发的辐射和热驱动器触发的流出模型。最大分辨率为$ 1.3 \ times 10^{ - 5} $ \，PC，并且在流入/流出的几何形状上没有限制。中央质量被认为是在$ z \ sim 15.9 $的红移中形成的{\ it之前}，并且可以构成$ \ sim 10^5 \，m_ \ odot $的超质量恒星（SMS），被成长的积分盘或自我加重的disk所包围。辐射转移是使用射线追踪算法建模的。由于$ \ sim 1 \，m_ \ odot \，{\ rm yr^{ - 1}} $的高积聚率，由DM Halo确定，积聚有些过度批评，导致了轻度的超临界亮度，导致对累积率的效果有限，对占名$ \ sim $ \ sim o \ sim \ sim o \ simber of sim of。我们观察到热腔的快速发展，该空腔迅速扩展到极性漏斗并扩大浓密的壳。在Funnels中，快风，$ \ sim 10^3 \，{\ rm km \，s^{ - 1}} $由积聚的气体批量加载。我们遵循扩展的外壳到$ \ sim 1 $ \，PC，当外壳速度保持大幅度时，$ \ sim 5 $ times，高于逃生速度。由中央UV/X射线形成的电离锥完全使腔体电离。推断流出属性表明，外壳外的光环材料将难以停止它。因此，我们得出的结论是，膨胀的风向壳将脱离中央parsec，并将到达光环病毒半径。最后，亚比sec量表上的各向异性积聚流将减弱h $ _2 $上的紫外线/软X射线。因此，funnels的形成和强大的外流，例如SMS可以具有有趣的观察性推论。
We use high-resolution zoom-in cosmological simulations to model outflow triggered by radiation and thermal drivers around the central mass accumulation during direct collapse within the dark matter (DM) halo. The maximal resolution is $1.3\times 10^{-5}$\,pc, and no restrictions are put on the geometry of the inflow/outflow. The central mass is considered {\it prior} to the formation of the supermassive black hole seed at a redshift of $z\sim 15.9$, and can constitute either a supermassive star (SMS) of $\sim 10^5\,M_\odot$ surrounded by a growing accretion disk or a self-gravitating disk. The radiation transfer is modeled using the ray-tracing algorithm. Due to the high accretion rate of $\sim 1\,M_\odot\,{\rm yr^{-1}}$ determined by the DM halo, accretion is mildly supercritical, resulting in mildly super-critical luminosity which has only a limited effect on the accretion rate, with the duty cycle of $\sim 0.9$. We observe a fast development of hot cavities, which quickly extend into polar funnels and expand dense shells. Within the funnels, fast winds, $\sim 10^3\,{\rm km\,s^{-1}}$, are mass-loaded by the accreting gas. We follow the expanding shells to $\sim 1$\,pc, when the shell velocity remains substantially, $\sim 5$ times, above the escape speed. The ionization cones formed by the central UV/X-ray completely ionize the cavities. Extrapolating the outflow properties shows that the halo material outside the shell will have difficulty stopping it. We therefore conclude that the expanding wind-driven shell will break out of the central parsec and will reach the halo virial radius. Finally, the anisotropic accretion flow on sub-parsec scales will attenuate the UV/soft X-rays on the H$_2$. Hence, the formation of funnels and powerful outflows around, e.g., SMS, can have interesting observational corollaries.
