AbstractA fundamental property of planetary magnetospheres, which varies from planet to planet, is the dynamical influence of either the solar wind and its embedded interplanetary magnetic field (IMF) or of the rotation of the planet. Jovian magnetospheric dynamics are mainly dominated by the combination of rapid planetary rotation and the outflow of material originating from the moon Io, orbiting deep within the magnetospheric cavity. The main auroral oval in Jupiter’s polar ionosphere appears fixed with respect to the planet, an indication of planetary control, and is understood to be associated with large-scale magnetosphere–ionosphere coupling, and the transfer of angular momentum from the ionosphere to the middle magnetosphere plasma. We will first discuss the origin of this main auroral oval, and the theoretical model which followed. We will also summarise recent developments of the theoretical model to include the effects of precipitation-induced enhancements of the ionospheric Pedersen conductivity in regions of upward field-aligned currents. Jupiter’s polar auroral emissions, which include all auroral emission lying poleward of the main auroral oval, are ordered by magnetic local time, indicating potential external control by the solar wind. We have recently considered from a theoretical standpoint what the effects of pulsed dayside magnetic reconnection will be at Jupiter. This will generate a twin-vortical flow pattern in the ionosphere across the open-closed field line boundary, associated with a bi-polar (i.e. upward and downward) field-aligned current pair. Here, we discuss the conditions under which such currents may be carried in either magnetospheric or cusp plasmas, and summarise the consequences for auroral emissions at UV and X-ray wavelengths.