论文标题
超级埃德丁顿政权如何影响高红色星系中的黑洞旋转进化
How the super-Eddington regime affects black hole spin evolution in high-redshift galaxies
论文作者
论文摘要
通过在孤立的暗物质光环中对星系进行三维流体力学模拟，我们遵循旋转参数$ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $涉嫌伴有强大的喷气流出的该制度有望降低BH旋转幅度。我们将超级 - 埃德丁顿积聚与亚埃德丁顿阶段（类星体和无线电模式）结合在一起，并遵循BH自旋进化。由于超级埃德丁顿发作的频率较低，因此在这种状态下，相对论的喷射无法有效地降低自旋的幅度，因为在类星体模式下薄的圆盘积聚不可避免地会增加BH旋转。由于超级 - 埃德丁顿事件的反馈，超级和亚埃德丁顿积聚的结合并不会导致自旋进化的简单表达。假设超级 - 埃德丁顿反馈始终弱，则可以使用分析表达式来计算$ a \ lyssim0.3 $的演变。最后，从低自旋幅度开始的BHS能够生长到最高的质量，如果它们最初开始与银河盘未对准，它们会通过逆行积聚获得少量积聚。
By performing three-dimensional hydrodynamical simulations of a galaxy in an isolated dark matter halo, we follow the evolution of the spin parameter $a$ of a black hole (BH) undergoing super-Eddington phases throughout its growth. This regime, suspected to be accompanied by powerful jet outflows, is expected to decrease the BH spin magnitude. We combine super-Eddington accretion with sub-Eddington phases (quasar and radio modes) and follow the BH spin evolution. Due to the low frequency of super-Eddington episodes, relativistic jets in this regime are not able to decrease the magnitude of the spin effectively, as thin disc accretion in the quasar mode inevitably increases the BH spin. The combination of super- and sub-Eddington accretion does not lead to a simple explicit expression for the spin evolution because of feedback from super-Eddington events. An analytical expression can be used to calculate the evolution for $a\lesssim0.3$, assuming the super-Eddington feedback is consistently weak. Finally, BHs starting with low spin magnitude are able to grow to the highest mass, and if they initially start misaligned with the galactic disc, they get a small boost of accretion through retrograde accretion.
