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基于全球三维磁层MHD(Magnetohydrodynamics)模拟模型,研究了行星际磁场(Interplanetary Magnetic Field,IMF)北向与南向时磁尾横断面(X=18 RE)的结构及等离子片的粒子注入机制.模拟结果很好地符合一些已知的观测数据和经验模型.从向阳面磁层顶IMF及重联后磁力线尾向运动过程的角度,对磁尾横断面粒子热压力分布、磁力线投影、等离子片或电流片旋转、粒子流场分布等结构进行了合理的解释.根据模拟得到的磁尾横断面结构,及IMF北向与南向时磁力线投影显著不同的位形,可以通过E×B漂移很好地说明不同IMF条件下,太阳风粒子对磁尾等离子片的不同注入特性.另外,还通过磁尾横断面磁场梯度的计算,说明了太阳风向等离子片粒子注入的晨-昏不对称性.
Based on the global three-dimensional Magnetohydrodynamics (MHD) simulation model, the structure of the magnetic tail cross section (X = 18 RE) along the north and south of the Interplanetary Magnetic Field (IMF) and the particle injection mechanism of the plasma sheet were studied. The results are in good agreement with some known observational data and empirical models. From the perspective of the magnetostrictive IMFs on the sunward side and the tail-end motion of the magnetic force lines after reconnection, the distributions of thermal stress, magnetic field lines, Current slice rotation and particle flow field distribution, etc. According to the structure of the magnetic tail cross section and the significant different projection of the magnetic line projection of the IMF northward and southward, the E x B drift can be well represented The different injection characteristics of the solar wind particles to the magnetic tail plasma sheet under different IMF conditions are described, and the morning-dusk asymmetry of the solar wind plasma sheet particle injection is also illustrated through the calculation of the magnetic tail cross-section magnetic field gradient.