Earth's magnetosheath forms the interface between our planetary magnetosphere and the supermagnetosonic solar wind flow. The magnetosheath is bounded by the bow shock separating it from the upstream solar wind, and by the magnetopause, which is the outer boundary of the magnetosphere. An important factor determining the nature of the bow shock and the magnetosheath is the orientation of the interplanetary magnetic field (IMF). Where the bow shock normal direction is quasi-parallel to the IMF, solar wind particles reflected at the bow shock can stream back toward the Sun, forming the turbulent foreshock upstream of the shock (e.g., Eastwood et al., 2005;Hoppe et al., 1981). Consequently, the magnetosheath behind the quasi-parallel bow shock is more turbulent (e.g., Dimmock et al., 2014;Gutynska et al., 2015) than the quasi-perpendicular magnetosheath. In recent years, one of the most important avenues in magnetosheath research has been the study of magnetosheath jets (e.g., Plaschke et al., 2018), which are regions of high dynamic pressure. Magnetosheath jets are widely associated with the quasi-parallel magnetosheath
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