  This study presents 3D resistive Hall-magnetohydrodynamic numerical
simulations focusing on the Kelvin-Helmholtz instability (KHI) dynamics at
Earth's magnetospheric flanks during northward interplanetary magnetic field
(IMF) periods. Through a comparative analysis of two simulations, we explore
the impact of distinct magnetic field orientations on plasma dynamics and
magnetic reconnection events. In one configuration, a uniform magnetic field
results in (double) Mid-Latitude Reconnection (MLR), while in the second
configuration, a magnetic shear induces both Type I Vortex Induced Reconnection
and MLR. Key findings include the symmetries and asymmetries in the latitudinal
distribution of KHI vortices and current sheets and a quantitative comparison
of reconnection events. Particularly noteworthy is the quantification of newly
closed field lines that experienced double reconnection, ultimately becoming
embedded in solar wind plasma at low latitudes while remaining connected to
magnetospheric plasma at high latitudes. The varying abundance of such lines in
the two simulations holds implications for plasma transport at the
magnetopause. This work significantly advances our understanding of
magnetospheric processes, emphasizing the essential role of a three-dimensional
perspective in accurately simulating magnetospheric plasma phenomena.

Space Physics;Solar and Stellar Astrophysics;Plasma Physics