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The overall focus on the driver of toroidal Pc5 waves has been on processes located at or\udacting on the dayside magnetopause and dayside flanks of the magnetosphere. These\udprocesses can generate waves that propagate tailward in the magnetosphere. However, an\udincreasing number of studies, both theoretical and experimental, have looked at waves\udpropagating sunward and that are caused by processes in the magnetotail. Here we present\udan ultra low frequency (ULF) wave observed in the post-midnight/morning sector of the\udmagnetosphere at L=16 RE. The wave has a toroidal mode polarization. We estimate\udthe azimuthal wave number to m=3, consistent with a toroidal mode type pulsation. The\udpositive sign indicates that the wave is propagating sunward and this is confirmed by\udlooking at the Poynting flux of the wave. The frequency of the wave is not constant with\udtime but shows a small increase in the beginning of the event up to over 2.0 mHz. Then\udthe frequency decreases to 1.0 mHz. This decrease coincides with a drop in the total\udmagnetic field strength and we speculate if this is related to an observed reversal of\udthe sign of the interplanetary magnetic field (IMF) By-component. This event occurs\udduring relatively quiet magnetospheric conditions with a solar wind speed of\udapproximately 400 km/s. Thus this event is highly likely to be driven by a source in the\udmagnetotail and the change in frequency is an excellent example that the frequency of an\udULF wave may be modulated by changes of the plasma parameters on the resonant field line

Sunward propagating Pc5 waves observed on the post-midnight magnetospheric flank