星系团近核区感生等离子体动力学的二维磁流体动力学模拟
2-D Magnetohydrodynamic Simulations of Induced Plasma Dynamics in the Near-Core Region of a Galaxy Cluster
摘要：
我们目前的结果，从数值模拟的冷却核心集群A2199产生的二维（2-D）的电阻磁流体动力学（MHD）的代码MH 2。在我们的模拟中，我们探讨了各向异性热传导对系统能量平衡的影响。在2-D轴对称几何的理想情况下的结果强调了ICM模拟中的初始等离子体密度的重要性，特别是近核心的值，因为辐射冷却率是成正比的${n_e}^2$。热传导被发现是无效的，在防止灾难性的冷却在这个集群。此外，我们进行了2-D平面MHD模拟从初始条件故意违反ICM中的热平衡和流体静力平衡，以评估对流项对各向异性热传导系统的能量平衡的贡献。我们发现，在这种情况下，工作所做的压力等离子体可以主导的各向异性热传导的内能在亚音速流的存在下，从而减少了影响的磁场的早期演变。星系团核心附近流体静力平衡的偏离可能与中央活动星系核的瞬态活动和/或ICM中的残余动力学活动有关，并需要进一步的三维研究。
英文摘要：
We present results from numerical simulations of the cooling-core cluster A2199 produced by the two-dimensional (2-D) resistive magnetohydrodynamics (MHD) code MACH2. In our simulations we explore the effect of anisotropic thermal conduction on the energy balance of the system. The results from idealized cases in 2-D axisymmetric geometry underscore the importance of the initial plasma density in ICM simulations, especially the near-core values since the radiation cooling rate is proportional to ${n_e}^2$. Heat conduction is found to be non-effective in preventing catastrophic cooling in this cluster. In addition we performed 2-D planar MHD simulations starting from initial conditions deliberately violating both thermal balance and hydrostatic equilibrium in the ICM, to assess contributions of the convective terms in the energy balance of the system against anisotropic thermal conduction. We find that in this case work done by the pressure on the plasma can dominate the early evolution of the internal energy over anisotropic thermal conduction in the presence of subsonic flows, thereby reducing the impact of the magnetic field. Deviations from hydrostatic equilibrium near the cluster core may be associated with transient activity of a central active galactic nucleus and/or remnant dynamical activity in the ICM and warrant further study in three dimensions.
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。
