The energetic charged particles penetration in the plasmasphere are carried out using the updated version of 3D Stanford PIC code. We considered slow and fast wind streams to know the penetration of the energetic charged particles (electrons and ions) having different velocities into four regions i.e. cusp, plasmasphere, sunward, and tailward sides. It is observed that the ion penetrations are higher than electrons for solar slow wind streams in the plasmasphere, while it is reverse for the solar fast streams. Also, the results show that the percentage of penetration of the energetic charged particles (both electrons and ions) are the same into the cusp and subsolar point reconnection region. It is different for the higher speed of fast streams; so that the penetrated electrons reached about 10–20 times than penetrated ions. The results show that for the tailward reconnection region, the penetration of ions is 2–3 times higher than the penetration of electrons, but it is the same for the case of higher solar fast speed.

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IMF向南期间磁层中带电粒子的渗透和分布的数值研究

使用3D Stanford PIC代码的更新版本进行等离子层中高能带电粒子的渗透。我们考虑了慢风和快风，以了解具有不同速度的高能带电粒子（电子和离子）向四个区域的渗透，即尖角，等离子层，向阳和向后的侧面。可以观察到，对于等离子层中太阳缓慢风流而言，离子渗透率高于电子，而对于太阳快速流而言则相反。而且，结果表明，高能带电粒子（电子和离子）进入尖端和太阳下点重新连接区域的渗透百分比相同。快速流的更高速度则有所不同。因此，所渗透的电子约为所渗透离子的10至20倍。