标题： 磁压主导稳定活动星系核盘对抗引力不稳定性 显示英文标题

标题： Magnetic Pressure Dominance Stabilizes AGN Disks Against Gravitational Instability

摘要： 磁性效应长期以来被认为可能是稳定活动星系核(AGN)吸积盘外区免受引力不稳定性(GI)影响的一个可能因素。 然而，测试这一假设的计算需求阻碍了对这个问题的全面研究。 在此，我们呈现了一套6个等温磁流体动力学(MHD)剪切盒模拟的结果，其中3个初始化为强磁化($\beta^{\rm{mid}}_{0} = p_{\rm{gas}} / p_{\rm{mag}} = 10^{2.5}$)，3个初始化为弱磁化($\beta^{\rm mid}_{0} = 10^{4}$)。 对于每种磁化情况，我们进行了强($Q_{0} = 1.0$)和弱($Q_{0} = 10.0$)自引力的模拟，其中 $Q_{0} = \frac{c_{\rm{s}}\Omega}{\pi G \Sigma_{0}}$是Toomre稳定性参数；我们还进行了纯MHD模拟以进行比较。 我们发现，我们的强磁化盘在初始化为临界稳定性后稳定免受GI影响，而相应的弱磁化盘则没有。 我们表明，强磁化、强自引力的盘主要由磁压主导，这导致了它的稳定。 显示英文摘要

摘要： Magnetic effects have long been considered a possible factor in stabilizing the outer regions of active galactic nuclei (AGN) accretion disks against gravitational instability (GI). However, the computational demands of testing this hypothesis have prevented comprehensive study of this problem. Here, we present results from a suite of 6 isothermal magnetohydrodynamics (MHD) shearing box simulations, 3 initialized with strong magnetization ($\beta^{\rm{mid}}_{0} = p_{\rm{gas}} / p_{\rm{mag}} = 10^{2.5}$) and 3 initialized with weak magnetization ($\beta^{\rm mid}_{0} = 10^{4}$). For each magnetization, we performed simulations with both strong ($Q_{0} = 1.0$) and weak ($Q_{0} = 10.0$) self-gravity, where $Q_{0} = \frac{c_{\rm{s}}\Omega}{\pi G \Sigma_{0}}$ is the Toomre stability parameter; we also performed pure MHD simulations for comparison. We find that our strongly magnetized disk stabilized against GI after initialization to critical stability against GI, while our corresponding weakly magnetized disk did not. We show that the strongly magnetized, strongly self-gravitating disk became dominated by magnetic pressure, which led to its stabilization.