具有大电阻率的电阻性MHD射流模拟
Resistive MHD jet simulations with large resistivity
摘要：
采用NIRVANA程序对径向自相似初始条件下的轴对称电阻磁流体动力学进行了数值模拟。磁扩散率可能发生在吸积盘上方的外流中，通过MHD湍流（异常湍流扩散率）从底层盘转移到盘冠中，或者作为部分电离流中的双极扩散的结果。我们介绍，除了经典的磁雷诺数Rm，它衡量的电阻效应的重要性，在感应方程，一个新的数字Rb，它衡量的电阻效应的重要性，在能量方程。我们在模拟中发现了两种不同的解决方案。一个是低电阻率制度，在其中的结果没有太大的不同，从理想的MHD解决方案。在高电阻率区，结果似乎显示出一些周期性的时间演化，并偏离理想的MHD的情况下显着。这种偏离是否是由数值或物理原因引起的，对数值模拟和天体物理外流理论有相当大的兴趣，目前正在研究。
英文摘要：
Axisymmetric resistive MHD simulations for radially self-similar initial conditions are performed, using the NIRVANA code. The magnetic diffusivity could occur in outflows above an accretion disk, being transferred from the underlying disk into the disk corona by MHD turbulence (anomalous turbulent diffusivity), or as a result of ambipolar diffusion in partially ionized flows. We introduce, in addition to the classical magnetic Reynolds number Rm, which measures the importance of resistive effects in the induction equation, a new number Rb, which measures the importance of the resistive effects in the energy equation. We find two distinct regimes of solutions in our simulations. One is the low-resistivity regime, in which results do not differ much from ideal-MHD solutions. In the high-resistivity regime, results seem to show some periodicity in time-evolution, and depart significantly from the ideal-MHD case. Whether this departure is caused by numerical or physical reasons is of considerable interest for numerical simulations and theory of astrophysical outflows and is currently investigated.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
