Shortly before the event the solar wind speed dropped from a maximum of 380
km/s to a steady value of 
throughout the event. IMF conditions
remained constant before and during the event with 
and 
positive and 
negative and magnitudes below 
. IMP8 was situated
within the magnetosphere.
The 
index at the time of the event was 4.0 (disturbed).
The overview in Figure 5.28 shows a localized region
of double-peaked spectra
from 
N to 
N except for a gap of some 
in longitude
from 
E to 
E.
Even when the rules are relaxed to allow for peaks with
a separation of up to 
, no more events are found in this region.
Figure 5.28: Map of spectral findings from the Saskatoon and Kapuskasing radars:
16 Jan/95
As can be seen in Figure 5.29, the satellite passes through
the longitudinal gap in the region of double-peaked spectra.
From 
to 
, the satellite traverses the latitude range
where double-peaked spectra occur to the east and west of the trajectory.
Figure 5.29: Peak-map with overlaid flight path of the DMSP F12 satellite: 16
Jan/95
Figure 5.30 shows that there was a very small flux during
most of the satellite track segment, except after 
.
The average energy is first low and after 
rises to about 
.
Figure 5.30: Average electron energy and flux determined from SSJ/4 instrument
measurements: 16 Jan/95
The ionization rate data shown in Figure 5.31 yield a more
revealing picture than the energy/flux data from the
previous figure. Observable is an increase in F-layer ionization by two
orders of magnitude from 
to 
,
corresponding approximately to the latitudes where double-peaked
spectra are found et higher and lower longitudes. The high energy electron
precipitation after is reflected in the increased E-layer ionization
rate and the E-layer conductivities that are presented in
Figure 5.32.
Figure 5.31: Estimated ionization rates at E- and F-layer heights determined from electron
spectra measurements: 16 Jan/95
Figure 5.32: Estimated E-layer conductivities from the Robinson model: 16 Jan/95
The velocity map in Figure 5.33 shows relatively high velocities and two
segments of flow in opposite directions, the dividing line along
N latitude, which is
approximately the position of double-peaked spectra.
Also notable is a region of low, randomly-directed velocities
around 
E and 
N. This is also the location
of an accumulation of double-peaked spectra observations.
Figure 5.33: SuperDARN velocity map: 16 Jan/95