Steady Models of Optically Thin, Magnetically Supported Black Hole Accretion Disks
Steady Models of Optically Thin, Magnetically Supported Black Hole Accretion Disks
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DOI：
10.1093/pasj/59.2.457
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发表时间：
2007-01
影响因子：
2.3
通讯作者：
H. Oda;M. Machida;K. Nakamura;R. Matsumoto
中科院分区：
文献类型：
--
作者：
H. Oda;M. Machida;K. Nakamura;R. Matsumoto
假设热轫致辐射冷却，我们获得了光学薄、单温、磁化黑洞吸积盘的稳定解。根据吸积盘 3D MHD 模拟的结果，我们假设吸积盘内部的磁场是湍流的，并且由方位角分量主导。我们将磁场分解为方位角平均场和脉动场。我们还假设方位平均麦克斯韦应力与总压力成比例。方位磁通量的径向平流率 P Φ 与 $ � � 成正比，其中 $ 是径向坐标
We obtained steady solutions of optically thin, single-temperature, magnetized black hole accretion disks, assuming thermal bremsstrahlung cooling. Based on the results of 3D MHD simulations of accretion disks, we assumed that the magnetic fields inside the disk are turbulent and dominated by an azimuthal component. We decomposed the magnetic fields into an azimuthally averaged mean field and fluctuating fields. We also assumed that the azimuthally averaged Maxwel ls tress i sp roportional to the total pressure. The radial advection rate of the azimuthal magnetic flux, P Φ ,i s prescribed as being proportional to $ � � ,w here$ is the radial coordinate