吸积盘中对流引起的湍流粘性--自洽方法
Turbulent viscosity by convection in accretion discs - a self-consistent approach
摘要：
天体物理吸积流中粘性的来源至今仍是一个争论激烈的问题。我们调查的对流湍流的贡献，总粘度在自洽的方法，对流的强度是由垂直盘结构本身。其他来源的粘度参数化的β-粘度处方，这也允许调查的自引力效应。在恒星质量和中等质量黑洞周围的吸积盘的背景下，我们得出结论，对流不能单独占总粘度在光盘，但显着增加到it.For吸积率高达10%的爱丁顿率，我们发现，差分旋转提供了一个足够大的基础粘度。对于更高的吸积率，需要进一步的支持，在内部磁盘区域，这可以提供由MRI引起的粘度。我们简要地讨论了MRI，对流和微分旋转的相互作用。我们对中心质量和吸积率对盘模型的影响进行了详细的参数研究，发现支撑粘性的阈值主要由爱丁顿比决定，中心黑洞质量的影响很小。
英文摘要：
The source of viscosity in astrophysical accretion flows is still a hotly debated issue. We investigate the contribution of convective turbulence to the total viscosity in a self-consistent approach, where the strength of convection is determined from the vertical disc structure itself. Additional sources of viscosity are parametrized by a beta-viscosity prescription, which also allows an investigation of self-gravitating effects. In the context of accretion discs around stellar mass and intermediate mass black holes, we conclude that convection alone cannot account for the total viscosity in the disc, but significantly adds to it. For accretion rates up to 10% of the Eddington rate, we find that differential rotation provides a sufficiently large underlying viscosity. For higher accretion rates, further support is needed in the inner disc region, which can be provided by an MRI-induced viscosity. We briefly discuss the interplay of MRI, convection and differential rotation. We conduct a detailed parameter study of the effects of central masses and accretion rates on the disc models and find that the threshold value of the supporting viscosity is determined mostly by the Eddington ratio with only little influence from the central black hole mass.
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