The magnetosheath is defined as the plasma region between the bow shock, where the super-magnetosonic solar wind plasma is decelerated and heated, and the outer boundary of the intrinsic planetary magnetic field, the so-called magnetopause. Based on the Soucek–Escoubet magnetosheath flow model at the Earth, we present an analytical magnetosheath plasma flow model around Mercury. The model can be used to estimate the plasma flow magnitude and direction at any given point in the magnetosheath exclusively on the basis of the plasma parameters of the upstream solar wind. The model serves as a useful tool to trace the magnetosheath plasma along the streamline both in a forward sense (away from the shock) and a backward sense (toward the shock), offering the opportunity of studying the growth or damping rate of a particular wave mode or evolution of turbulence energy spectra along the streamline in view of upcoming arrival of BepiColombo at Mercury.

中文翻译：

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水星周围的磁鞘等离子体流模型

磁鞘被定义为弓形激波（超磁声太阳风等离子体在此处减速和加热）与行星固有磁场的外边界（即所谓的磁层顶）之间的等离子体区域。基于地球上的 Soucek-Escoubet 磁鞘流模型，我们提出了一个围绕水星的分析磁鞘等离子体流模型。该模型可用于仅根据上游太阳风的等离子体参数来估计磁鞘中任何给定点的等离子体流大小和方向。该模型是一种有用的工具，可以在向前（远离激波）和向后（向激波）方向上沿着流线追踪磁鞘等离子体，