Magnetohydrodynamic Numerical Simulation of Parker Instability in Interstellar Gas with Cosmic Ray Pressure
Magnetohydrodynamic Numerical Simulation of Parker Instability in Interstellar Gas with Cosmic Ray Pressure
复制标题
DOI：
10.7566/jpscp.1.015105
复制
发表时间：
2014-03
期刊：
影响因子：
--
通讯作者：
T. Kudoh;T. Yokoyama;R. Matsumoto
中科院分区：
文献类型：
--
作者：
T. Kudoh;T. Yokoyama;R. Matsumoto
本文对银盘中存在宇宙线压力的帕克不稳定性进行了二维MHD数值模拟。而不是对称的边界条件上的银道面经常使用，我们解决了整个地区的磁盘。在线性阶段，当宇宙线压力较大时，盘上的对称模也增长，而当宇宙线压力较小时，盘上的滑移反射对称模占主导地位。在非线性阶段，当宇宙线压力较大时，磁力线的某些环结构迅速膨胀并长大为大结构。其他循环，开始增长稍晚，被位于附近的快速增长的循环抑制，并且没有达到非线性扩展。最终，当宇宙线压力相对较大时，非线性阶段的环结构与线性阶段的环结构并不一致。
We perform two-dimensional MHD numerical simulations of the Parker instability with the cosmicray pressure under the circumstance of the galactic disk. Instead of the symmetric boundary conditions on the galactic plane as often used, we solve the entire region of the disk. In the linear stage, the symmetric mode on the disk also grows when the cosmic-ray pressure is large, while the glide reflection symmetric mode dominates on the disk when the cosmic-ray pressure is small. In the nonlinear stage, some loop structures of the magnetic field lines expand rapidly and grow into large structure when the cosmic-ray pressure is large. Other loops, which start to grow a little later, are suppressed by faster growing loops located nearby and do not reach the nonlinear expansions. Eventually, the loop structure at the nonlinear stage does not coincides with that at the linear stage when the cosmic-ray pressure is relatively large.