Only observations outside of the SAA are included. The number varies by approximately a factor of 2 from the low to high geomagnetic lattitude. No significant trend is evident. Figure 3 shows the ratio of the number of cosmic ray pixels divided by the number of cosmic ray events detected. The event affects approximately 4 pixels.
Some variation is evident with geomagnetic latitude.
However, this variation may be just the fact that at higher latitudes multiple events are more likely to occur near each other on the detector and get counted as a single event. Figure 4 shows the center locations of the nineteen 60 second darks taken during a SAA passage. Figure 5 shows the number of events detected and figure 6 the number of pixels affected in each of the SAA observations. The flat top on the profile in figure 5 is probably caused by the significant confusion of events. Figure 6 gives a more realistic measure of the variation in the number of events during the SAA passage.