Solar Wind Control of the Martian Magnetotail Current Sheet and Magnetic Reconnection

Abstract Magnetic reconnection is a rapid process that releases magnetic free energy stored in current sheets (CSs), driving various explosive phenomena throughout the Universe. In planets within the solar system, reconnection is controlled by both the solar wind and the planet’s magnetic field and rotation. In this study, we perform a statistical analysis of the characteristics of CSs and reconnection events in the Martian magnetotail, considering varying solar wind conditions and local crustal field variations. The results show that higher solar wind dynamic pressure leads to a significantly increased probability of reconnection, primarily due to the enhanced cross-tail current density. In contrast, the orientation of interplanetary magnetic fields and local crustal anomalies predominantly affect the spatial distribution of CSs and reconnection events. Moreover, high solar wind dynamic pressure significantly enhances the average tailward flux of hydrogen and oxygen ions, likely attributable to the enhanced pickup of planetary ions.