Abstract Non-adiabatic energization and transport of planetary ions in the vicinity of Kelvin-Helmholtz (KH) vortices at Mercury are statistically investigated using a magnetohydrodynamic model combined with a test particle tracing technique. The measurements from the MErcury Surface, Space ENvironment, Geochemistry, and Ranging spacecraft show signatures of KH waves in the magnetospheric flanks, especially on the duskside. We examine here the energization and transport of heavy ions of planetary origin such as Na + associated with the growth of the KH instability on both the dawn and dusk sides of the magnetosphere, and for both northward and southward interplanetary magnetic field configurations. We find that in all cases those planetary ions in the magnetosphere can be accelerated non-adiabatically with a level of acceleration larger on the dawnside. The transport of those ions is controlled by the convection electric field in the magnetosheath. Those planetary ions when picked up in the duskside magnetosphere where the KH waves have been mainly observed at Mercury stagnate inside the magnetosphere and, hence, are not expected to escape. The present study indicates that these ions may likely stay inside the magnetosphere and sputter the planetary surface on the duskside preferentially, being the source of secondary neutrals from the planetary surface.

中文翻译：

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水星开尔文-亥姆霍兹涡流中非绝热激发和输运的统计研究

摘要 使用磁流体动力学模型结合测试粒子追踪技术，对水星开尔文-亥姆霍兹 (KH) 涡流附近行星离子的非绝热激励和传输进行了统计研究。来自汞表面、空间环境、地球化学和测距航天器的测量结果显示了磁层侧翼 KH 波的特征，尤其是在黄昏时分。我们在这里研究了与磁层黎明和黄昏两侧 KH 不稳定性的增长以及向北和向南行星际磁场配置相关的行星起源的重离子（例如 Na + ）的激发和传输。我们发现，在所有情况下，磁层中的这些行星离子都可以非绝热地加速，黎明侧的加速水平更大。这些离子的传输由磁鞘中的对流电场控制。这些行星离子在黄昏磁层中被拾取时，主要在水星上观察到 KH 波在磁层内停滞，因此预计不会逃逸。目前的研究表明，这些离子可能会留在磁层内部，并优先在黄昏的行星表面溅射，成为行星表面二次中性粒子的来源。这些行星离子在黄昏磁层中被拾取时，主要在水星上观察到 KH 波在磁层内停滞，因此预计不会逃逸。目前的研究表明，这些离子可能会留在磁层内部，并优先在黄昏的行星表面溅射，成为行星表面二次中性粒子的来源。这些行星离子在黄昏磁层中被拾取时，主要在水星上观察到 KH 波在磁层内停滞，因此预计不会逃逸。目前的研究表明，这些离子可能会留在磁层内部，并优先在黄昏的行星表面溅射，成为行星表面二次中性粒子的来源。