WIND measured a slight increase of the solar plasma speed from 310 to 320 km/s along with a change of and from zero to a small positive value around the time the event was recorded. IMF conditions were undisturbed otherwise. IMP8 IMF measurements compare well with the WIND measurements. The index at the time of the event was 1.0.
Figure 5.34 shows that backscatter was observed by both radars from an extended region. The Kapuskasing radar, however, shows an echo gap from E to E, centered at a latitude around N. A patch of double-peaked spectra was observed mostly by the Kapuskasing radar from E to E at a latitude around N.
Figure 5.34: Map of spectral findings from the Saskatoon and Kapuskasing radars: 26 Jan/95
In Figure 5.35 the satellite track for this event is shown; one can identify two regions. First, coming from the north, the satellite passes by the double-peaked spectra region at about . It then enters the region of missing backscatter from the Kapuskasing radar at and leaves it again at .
Figure 5.35: Peak-map with overlaid flight path of the DMSP F12 satellite: 26 Jan/95
The flux and energy data in Figure 5.36 also show two regions. From 59185 s to there is increased flux of electrons. Then, from 59235 s there is an increased flux of electrons until , then of electrons until , followed by electron energies of or more - all relatively high electron energies.
Figure 5.36: Average electron energy and flux determined from SSJ/4 instrument measurements: 26 Jan/95
The ionization rates shown in Figure 5.37 compare well with the radar observations in the fact that there exists a region of high F-layer ionization which is centered around , the time when double-peaked spectra were observed.
Figure 5.37: Estimated ionization rates at E- and F-layer heights determined from electron spectra measurements: 26 Jan/95
Figure 5.38 shows the E-layer conductivities, which are small, reflecting the low flux in the precipitation pattern. A sharp gradient in the conductances is observed at .
Figure 5.38: Estimated E-layer conductivities from the Robinson model: 26 Jan/95
As in the event on 16 Feb/95, Figure 5.39 shows a velocity map that is dominated by flow in opposite directions. The region of the convection reversal corresponds reasonably well to the location of the double peaked spectra.
Figure 5.39: SuperDARN velocity map: 26 Jan/95