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分析了Helios高分辨率数据 ,找到太阳风湍动中可能发生磁重联过程的观测事例 ,并将空气动力学中的三阶精度迎风紧致差分格式引入可压缩的二维磁流体动力学 (MHD)中 ,数值模拟研究行星际太阳风中这种小尺度湍动磁重联现象 .主要新结果是 :行星际太阳风中湍动磁重联过程可以发生 ;湍动磁重联是高磁Reynolds数 (RM=2 0 0 0 ,1 0 0 0 0 )太阳风中磁重联的基本特征 ,磁重联多由单X射线重联向多X射线重联发展 ;磁岛的不断形成、合并与演化十分复杂 ,最终将向低能态状态演化 ;不同演化阶段、不同穿越路径 ,将有很不相同的磁场、流场信号记录 .小尺度湍动磁重联的数值实验结果可从原理上解释飞船观测结果 ,有助于揭示太阳风基本物理过程
The Helios high-resolution data was analyzed to find out the observed cases of magnetic reconnection process in the solar wind turbulence. The third-order precision windward compact finite difference scheme in aerodynamics was introduced into compressible two-dimensional magnetohydrodynamics (MHD ), A numerical simulation of this small-scale turbulent magnetic reconnection in interplanetary solar wind is presented. The main new result is that turbulent magnetic reconnection can occur in interplanetary solar winds; turbulent magnetic reconnections are highly magnetic Reynolds numbers RM = 2000, 1 0 0 0 0) The basic characteristics of magnetic reconnection in the solar wind are mostly reconnected with single X-ray to multiple X-ray reconnection. The continuous formation, merger and evolution of magnetic islands Complex and will eventually evolve to a low energy state.Different stages of evolution and different paths of crossing will result in very different magnetic and flow field signals.Numerical experimental results of the small-scale turbulent magnetic reconnection can explain the spacecraft observations in principle , Helps to reveal the basic physical processes of the solar wind