论文标题
MHD积聚：喷气机由非异分积聚磁盘发电机发射。 ii。由磁盘coriolis编号定义的发电机张量
MHD accretion-ejection: jets launched by a non-isotropic accretion disk dynamo. II. A dynamo tensor defined by the disk Coriolis number
论文作者
论文摘要
天体物理喷气机是从强大的磁化系统发射的，该系统围绕着中心物体的积聚盘。在这里，我们解决了如何生成喷气发射所需的积聚磁盘磁化和现场结构的问题。我们从纸I（Mattia＆Fendt 2020a）中继续工作，考虑到大型磁盘示例的非量表积聚磁盘平均场$α^2Ω$ -DONNAMO。现在，我们研究了一个磁盘发电机，该磁盘发电机遵循平均场扰动理论的分析解，本质上仅基于单个参数，即科里奥利数。因此，我们确认发挥作用在吸积盘中的发电机张量的各向异性，从而使电阻率和均值发电机与磁盘湍流相关联。我们的新模型恢复了使用纯粹的径向初始场的先前模拟，同时允许对具有垂直分量的种子场进行更稳定的进化。我们还介绍了磁盘发电机系数的强度与发射的射流的动力学参数之间的相关性，并讨论了它们对观察到的射流量的影响。
Astrophysical jets are launched from strongly magnetized systems that host an accretion disk surrounding a central object. Here we address the question how to generate the accretion disk magnetization and field structure required for jet launching. We continue our work from Paper I (Mattia & Fendt 2020a), considering a non-scalar accretion disk mean-field $α^2Ω$-dynamo in the context of large scale disk-jet simulations. We now investigate a disk dynamo that follows analytical solutions of mean-field dynamo theory, essentially based only on a single parameter, the Coriolis number. We thereby confirm the anisotropy of the dynamo tensor acting in accretion disks, allowing to relate both the resistivity and mean-field dynamo to the disk turbulence. Our new model recovers previous simulations applying a purely radial initial field, while allowing for a more stable evolution for seed fields with a vertical component. We also present correlations between the strength of the disk dynamo coefficients and the dynamical parameters of the jet that is launched, and discuss their implication for observed jet quantities.
