论文标题
超级埃德丁顿积聚流向黑洞，伴随着强大的流出
Hyper-Eddington accretion flows onto black holes accompanied by powerful outflows
论文作者
论文摘要
我们对Protogalaxies核对黑洞（BHS）进行增生流动的二维辐射流体动力学模拟，并研究机械和辐射反馈对BHS快速生长的影响。流出将质量，动量和能量沉积到周围的培养基中，并防止质量积聚到BH上，从而减少辐射输出。我们发现，当BH嵌入密集的气体芯中时，由于机械反馈而效率低下的BH喂养降低了电离辐射，这几乎不会影响BH重力的影响范围的气体动力学，从而在埃德丁顿（Eddington）限制的情况下，中性气的强烈流入从中出现，而中性气体的强烈流入发生，而没有照相和热量影响。由于迅速吸收的BH驱动的流出的机械功率足够强，因此双极外流完全撤离了极地地区的周围气体，但是质量在赤道区域中流动的质量在赤道区域中涌入高达$ \ sim 300-10-10^3〜 \ dot {m} _ {m} _ {\ rm edd} $ radiive tress n of tress n of tress n of tress n of tress n offect from rm vertive tress。此外，我们发现快速积聚所需的临界气体密度降低了$ \ sim 3 $几乎独立于BH质量的$ \ sim 3 $。通过研究对流出模型参数的依赖性（例如，开头角度，质量加载程度为流出，速度），我们得出结论，与天真的预期相反，存在更强的流出导致过渡到快速积聚阶段的过渡。快速生长的BHS以$ \ sim 0.1-1 \％$的辐射发光度注入机械功率，将其用于宿主星系尺度，用于宇宙学模拟。
We perform two-dimensional radiation hydrodynamical simulations of accretion flows onto black holes (BHs) at the nuclei of protogalaxies, and study the impact of mechanical and radiative feedback on rapid growth of BHs. The outflows deposit mass, momentum and energy into the surrounding medium and prevent mass accretion onto the BH, resulting in the reduction of radiative output. We find that when the BH is embedded in a dense gas core, ionizing radiation attenuated by inefficient BH feeding owing to mechanical feedback hardly affects the gas dynamics at the BH gravitational sphere of influence, from which intense inflows of neutral gas occur at rates substantially exceeding the Eddington limit without impeded by photoionization and heating. Since mechanical power of outflows driven by the rapidly accreting BH is sufficiently strong, bipolar outflows completely evacuate the surrounding gas in the polar region but mass inflows through the equatorial region maintain the BH accretion rate as high as $\sim 300-10^3~\dot{M}_{\rm Edd}$, which is reduced by one order of magnitude from those with radiative feedback alone. Furthermore, we find that the critical gas density required for rapid accretion is lower by a factor of $\sim 3$ nearly independently of BH mass, when mechanical feedback is considered. By studying the dependence on outflow model parameters (e.g., opening angle, mass-loading degree into outflows, velocity), we conclude that contrary to naive expectation, the existence of stronger outflow leads to the transition to rapid accretion phases more efficiently. Rapidly growing BHs inject mechanical power with $\sim 0.1-1\%$ of the radiative luminosity into their host galaxy scales, which is used for cosmological simulations.
