Mercury and Earth are the only inner planets to have strong internal magnetic fields and consequently have planetary magnetospheres (Russell et al., 1988). The overall structure of Mercury's magnetosphere is like Earth's in that a bow shock forms upstream of the magnetopause, cusps form at dayside high latitudes, and an elongated magnetotail with a plasma sheet forms (Slavin et al., 2008;Zurbuchen et al., 2011). Critically important processes involving particle kinetics such as magnetic reconnection, wave-particle interactions, and non-adiabatic particle motion strongly influence plasma transport, energization, and loss in planetary magnetospheres. Here, we present results from a global kinetic particle-in-cell (PIC) simulation to investigate the dynamics of Mercury's magnetosphere as a coupled, interacting kinetic system with ions and electrons treated self-consistently. We examine the effects of electron kinetics, which can be important for local-global space plasma physics processes (Verscharen et al., 2021), in the context of planetary magnetospheric dynamics.Mercury has the distinction of having the smallest planetary magnetosphere in our solar system (Kivelson & Russell, 1995;Russell et al., 1988). Mariner 10 data from the 1970s established that Mercury has an intrinsic magnetic field, and this inference has been confirmed by magnetic field observations from the Mercury Surface, Space Environment, Geochemistry and Ranging (MESSENGER) spacecraft (Anderson et al., 2008). The planet has a dipole moment of 250 nT R M 3 (where R M is Mercury's radius = 2439 km) and a tilt with respect to the planetary rotation axis of no more than 5° (