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This signal is also visible in the 1H ULF spectrum of 3,5-bis trifluoromethyl pyridine.
Pc 5 ULF waves are seen concurrently with the rise in radiation belt fluxes associated with CME magnetic cloud events.
Fig. 9 ULF dependence on AE and solar wind density.
Figure 5b shows the relative timing between the Pi1-2 and Pi1 ULF wave bands.
Figure 5b clearly demonstrates that the onset of Pi1-2 ULF waves occur ~ 1 4 min prior to the higher frequency Pi1 ULF waves, other than at one station (BRDN) which lies within the timing uncertainty contour.
We find that the Pi1-2 ULF wave band occurs first at auroral latitudes, but Pi2 ULF waves may be observed concurrently at lower latitudes, to within the timing uncertainty of the technique.
Both signals are presented in temporal and spectral domains in Figure 4. Figure 4 ULF sources: waveforms and spectrums.
Figure 3 shows exemplar AWESOME power spectra for the GILL magnetometer for six ULF wave bands spanning the Pi1 Pi2 ULF wave periods and starting at 0555 UT.
We present a case study of the relative timing of ULF wave onset across the Pi1 and Pi2 ULF wave bands.
In summary, it can be observed from Fig. 3 that ULF waves in the Pi1-2 band occur first at the GILL magnetometer, followed ~ 100 s later by the onset of waves in the traditional Pi2 and Pi1 ULF wave bands.
The onset of Pi1 ULF waves is delayed longest with respect to the onset of Pi1-2 wates athesese lowest observable latitudes.
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