标题： 太阳风进入水星磁层：贝皮可伦坡第二次飞越的模拟结果 显示英文标题

标题： Solar wind entry into Mercury's magnetosphere: Simulation results for the second swingby of BepiColombo

摘要： 上下文。 我们使用一个全局3D混合等离子体模型来研究水星磁层与太阳风在第二次贝皮可伦坡飞越期间的相互作用，评估磁层区域，并研究质子的典型能量分布。 目标。 本研究的目的是更好地理解太阳风进入情况，并利用第二次贝皮可伦坡飞越条件分析模拟的等离子体数据，以增强我们对测量数据的理解，并可能为未来的飞越提供预测。 方法。 为了模拟水星的等离子体环境，我们使用了混合代码AIKEF，并开发了一种方法来提取粒子（离子）数据，以计算2022年6月23日第二次水星飞越期间贝皮可伦坡轨迹上的质子能量谱。 我们在平均上游太阳风条件下评估磁层顶和弓激波的远离距离，其中地冕磁场（IMF）条件由第二次水星飞越期间贝皮可伦坡磁场测量得出。 结果。 我们发现，在弓激波的准垂直（黄昏）侧的磁鞘比准平行（黎明）侧更厚，在那里形成了前激波。 可以从我们模拟的能量谱中提取多种等离子体群体，有助于识别磁层区域。 我们观察到源自太阳风的质子进入水星磁层。 它们的能量范围从磁层中的几个电子伏特到磁鞘中的10 keV。 显示英文摘要

摘要： Context. We use a global 3D hybrid plasma model to investigate the interaction between Mercury's magnetosphere and the solar wind for the second BepiColombo swingby, evaluate magnetospheric regions, and study the typical energy profile of protons. Aims. The objective of this study is to gain a better understanding of solar wind entry and analyze simulated plasma data along a trajectory using BepiColombo swingby 2 conditions, with the goal of enhancing our comprehension of measurement data and potentially providing forecasts for future swingbys. Methods. To model Mercury's plasma environment, we used the hybrid code AIKEF and developed a method to extract the particle (ion) data in order to compute the proton energy spectrum along the trajectory of BepiColombo during its second Mercury swingby on June 23, 2022. We evaluate magnetopause and bow shock stand-off distances under average upstream solar wind conditions with the Interplanetary Magnetic Field (IMF) condition derived from the BepiColombo magnetic field measurements during the second Mercury swingby. Results. We found that the magnetosheath on the quasi-perpendicular (dusk) side of the bow shock is thicker than that on the quasi-parallel (dawn) side, where a foreshock is formed. Multiple plasma populations can be extracted from our modeled energy spectra that assist in identifying magnetospheric regions. We observed protons of solar wind origin entering Mercury's magnetosphere. Their energies range from a few electron volts in the magnetosphere up to 10 keV in the magnetosheath.