Turbulent Comptonization in Black Hole Accretion Disks
Turbulent Comptonization in Black Hole Accretion Disks
复制标题
黑洞吸积盘中的湍流康化化
DOI：
10.1086/380301
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发表时间：
2003
期刊：
影响因子：
--
通讯作者：
O. Blaes
中科院分区：
文献类型：
--
作者：
A. Socrates;S. Davis;O. Blaes
在辐射压力支持的吸积盘的最内部区域，湍流磁压力可能大大超过气体的磁压力。如果是这种情况，由磁旋转不稳定性（MRI）驱动的整体阿尔芬运动有可能超过电子热速度。那么，体积而不是热的康普顿化可能是介导重力能量释放的主要辐射过程。对于足够大的湍流应力，我们表明湍流康普顿化对黑洞吸积盘的远紫外和 X 射线发射产生了显着的贡献。该光谱分量的存在提供了一种获得对湍流本身性质的直接观测约束的方法。我们描述了该成分如何影响 X 射线双星和活动星系核 (AGN) 的光谱能量分布和变异特性。
In the innermost regions of radiation pressure-supported accretion disks, the turbulent magnetic pressure may greatly exceed that of the gas. If this is the case, it is possible for bulk Alfvénic motions driven by the magnetorotational instability (MRI) to surpass the electron thermal velocity. Bulk, rather than thermal, Comptonization may then be the dominant radiative process that mediates gravitational energy release. For sufficiently large turbulent stresses, we show that turbulent Comptonization produces a significant contribution to the far-UV and X-ray emission of black hole accretion disks. The existence of this spectral component provides a means of obtaining direct observational constraints on the nature of the turbulence itself. We describe how this component may affect the spectral energy distributions and variability properties of X-ray binaries and active galactic nuclei (AGN).