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Polarization Properties of 3‐D Field Line Resonances

Recent work has shown that field line resonances (FLRs) can form with intermediate magnetic field polarizations, that is, between toroidal (azimuthal) and poloidal (radial). In this case, they are referred to as “3‐D”, given that the equilibrium and therefore associated wave solutions vary in all three dimensions. Such 3‐D variations in the medium can be expected in the magnetosphere in particular during the presence of a plasmaspheric drainage plume in the dusk flank. In this case, strong field‐aligned currents driven by FLRs can form along contours of Alfvén frequency which are very asymmetric azimuthally. In this study, we use magnetohydrodynamic (MHD) simulations performed in a background dipole magnetic field, to consider what the satellite signatures would be for a spacecraft observing such non‐toroidal FLRs under different magnetopause driving conditions. We consider how the 3‐D nature impacts the amplitude and phase relations traditionally expected for FLRs. We find that in the 3‐D FLR regions of intermediate polarization, the FLR has strong contributions from both the radial and azimuthal field components (velocity, magnetic or electric) and these are in or out of phase. We show how hodograms can be used to infer the FLR polarization in these cases as well as provide predictions for the variation of the FLR polarization with MLT across a plasmaspheric plume. We further show how the presence of a significant global fast mode can skew the resulting polarization estimates.