论文标题
由薄积盘驱动的风力驱动的风的大规模动力学
Large-scale Dynamics of Winds Driven by Line Force from a Thin Accretion Disk
论文作者
论文摘要
风在主动银河核反馈过程中起着重要作用。先前研究风的模拟仅集中于小动力学范围。因此，尚不清楚风能可以走多远，如果风的特性可以移动到大半径。我们执行模拟来研究由线力驱动的风的大规模动力学。我们发现风的特性取决于黑洞质量（$ M_ {BH} $）和积聚磁盘光度。当积聚磁盘光度为$ 0.6L_ {EDD} $（$ l_ {edd} $是Eddington Luminosity），独立于$ M_ {BH} $，风能超过$ 1 \％L_ {EDD} $，并且可以从黑洞的电位中逃脱。对于带有积分磁盘光度等于0.3 $ l_ {edd} $的情况，风的强度随着$ m_ {bh} $的降低而降低。如果$ m_ {bh} $从$ 10^9 $减少到$ 10^6 $太阳质量（$ m_ \ odot $），则风能流量通量从$ \ sim 0.01 l_ {edd} $降低到$ \ $ \ sim 10^{-6} l_ eDd} $。如果$ m_ {bh} \ geq 10^7 m_ \ odot $，风可以从黑洞的潜力中逃脱。对于$ m_ {bh} = 10^6 m_ \ odot $，风无法逃脱。我们发现，对于在硬X射线带中观察到的超快速风（\ citealt {Gofford etal。2015}），观察到的质量通量的依赖性和动能通量对积聚磁盘的亮度可以很好地由线力驱动的风模型产生。我们还发现，可以通过线力驱动的风模型来解释在软X射线带中观察到的超快速风的性能。
Winds play a significant role in active galactic nuclei feedback process. Previous simulations studying winds only focus on a small dynamical range. Therefore, it is unknown how far the winds can go and what the properties of the winds will be if they can move to large radii. We perform simulations to study the large scale dynamics of winds driven by line force. We find that the properties of the winds depend on both black hole mass ($M_{BH}$) and accretion disk luminosity. When the accretion disk luminosity is $0.6L_{edd}$ ($L_{edd}$ being Eddington luminosity), independent of $M_{BH}$, the winds have kinetic energy flux exceeding $1\% L_{edd}$ and can escape from the black hole potential. For the case with the accretion disk luminosity equaling 0.3$L_{edd}$, the strength of the winds decreases with the decrease of $M_{BH}$. If $M_{BH}$ decreases from $10^9$ to $10^6$ solar mass ($M_\odot$), the winds kinetic energy flux decreases from $\sim 0.01 L_{edd}$ to $ \sim 10^{-6} L_{edd}$. In case of $M_{BH}\geq 10^7 M_\odot$, winds can escape from black hole potential. In the case of $M_{BH}=10^6 M_\odot$, the winds can not escape. We find that for the ultra-fast winds observed in hard X-ray bands (\citealt{Gofford et al. 2015}), the observed dependence of the mass flux and the kinetic energy flux on accretion disk luminosity can be well produced by line force driven winds model. We also find that the properties of the ultra-fast winds observed in soft X-ray bands can be explained by the line force driven winds model.
