AI 中文总结
通过32个广义相对论辐射磁流体动力学模拟，明确黑洞自旋与吸积率调控超爱丁顿磁化吸积的风损失率与能量输出效率，给出相关标度关系，为解释ULXs观测提供框架。
AI 中文摘要
强磁化超爱丁顿吸积流驱动着诸多重要天体物理系统，但黑洞参数如何调控其输出尚不明确。我们开展了32个针对恒星级黑洞超爱丁顿磁化吸积盘的广义相对论辐射磁流体动力学模拟，变量包括黑洞质量（$M_{\rm BH}=5、15、30M_{\rm \bigodot}$）、自旋（$a=0、0.9$）与吸积率（$\bar{M}_{\rm acc}\thickapprox1-2000\bar{M}_{\rm Edd}$）。研究发现，黑洞自旋与吸积率共同调控风损失率与能量输出效率，而在本次研究的质量范围内黑洞质量无影响。黑洞仅吸积供给吸积流质量的10%-40%，其余均以风的形式被抛射，该吸积占比随质量供给率降低，且高自旋系统的吸积占比更低。两种自旋状态均产生强磁化驱动外流：$a=0$时，风的动能、辐射与电磁效率适中，在全模拟吸积率范围内变化很小；$a=0.9$时，风功率与喷流功率均随$\bar{M}_{\rm acc}$超线性增长，且喷流功率在$\bar{M}_{\rm acc}\thicksim100\bar{M}_{\rm Edd}$后趋于饱和。辐射沿漏斗状结构强烈集束，高自旋、高$\bar{m}$模型正对观测时逆集束因子超100。本研究证实，快速黑洞自旋可提升能量提取效率，高吸积率可放大总功率，还给出了光度、喷流功率、吸积比与集束性的标度关系，为解释ULXs及其他超爱丁顿系统观测提供框架。
英文摘要
Strongly magnetized super-Eddington accretion flows power many important astrophysical systems, but how black hole parameters control their output is unclear. We present 32 general relativistic radiation magnetohydrodynamics simulations of super-Eddington magnetically arrested disks onto stellar-mass black holes, varying mass ($M_{\rm BH}= 5, 15, 30\,M_{\odot}$), spin ($a=0,0.9$), and accretion rate ($\dot{M}_{\rm acc} \approx 1-2000\,\dot{M}_{\rm Edd}$). We find that black hole spin and accretion rate jointly regulate wind loss rates and energy output efficiencies, while black hole mass has no effect over the mass range studied here. The BH accretes only $10-40\%$ of the mass supplied to the accretion flow, while the rest is expelled in winds. This accretion fraction decreases with mass supply rate and is lower for high-spin systems. Both spin states produce strong magnetically driven outflows. For $a = 0$, the wind kinetic, radiative, and electromagnetic efficiencies are modest and show little variation across the full simulated range of accretion rates. For $a = 0.9$, both wind power and jet power increase super-linearly with $\dot{M}_{\rm acc}$, with the jet power saturating beyond $\dot{M}_{\rm acc} \sim 100\,\dot{M}_{\rm Edd}$. Radiation is strongly beamed along the funnel, with inverse beaming factors exceeding $100$ for high-spin, high-$\dot{m}$ models viewed face-on. Our results establish that rapid BH spin boosts energy-extraction efficiency, while high accretion rate amplifies total power. We provide scaling relations for luminosities, jet power, accretion ratio, and beaming, offering a framework for interpreting observations of ULXs and other super-Eddington systems.
Comments15 main figures, 4 tables, submitted
