Disk modelling by radiationmagnetohydrodynamic simulations
Disk modelling by radiationmagnetohydrodynamic simulations
复制标题
通过辐射磁流体动力学模拟进行圆盘建模
DOI：
10.1051/epjconf/20123906005
复制
发表时间：
2012
期刊：
影响因子：
--
通讯作者：
Takeuchi,S
中科院分区：
文献类型：
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作者：
Mineshige;S.;Ohsuga;K.;Takeuchi,S
历史上，各种吸积模型已被讨论下径向单区近似。然而，在这种单区模型中，吸积流的动力学方面，如内循环和外流，被完全忽略了。此外，圆盘粘度通常由唯象α粘度模型描述。在这里，我们阐明吸积流和外流的理论的基础上，我们的全球，二维辐射磁流体动力学模拟，不依赖于α模型。我们已经成功地生产三种不同的状态的吸积流控制只有一个参数，密度归一化。特别重要的是，这三个州都存在外流现象。超临界（或超爱丁顿）吸积流的几个值得注意的特点被发现，即相对论性，准直流出（射流），低速，非准直流出的cluerical结构。观测的影响进行了简要讨论。
Historically, various accretion models have been discussed under radially one-zone approximations. In such one-zone models, however, dynamical aspects of the accretion flow, such as internal circulation and outflows, have been totally neglected. Further, the disk viscosity is usually described by the phenomenological α-viscosity model. We, here, elucidate the theory of accretion flows and outflows based on our global, two-dimensional radiation-magnetohydrodynamic simulations, not relying on the α model. We have succeeded in producing three distinct states of accretion flow by controling only one parameter, a density normalization. Of particular importance is the presence of outflows in all three states. Several noteworthy features of the supercritical (or super-Eddington) accretion flows are found; that is, relativistic, collimated outflows (jets), and low-velocity, uncollimated outflows with clumpy structure. Observational implications are briefly discussed.