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Fig. 14

image

a) Onset time delays of 55–65 keV electrons relative to the type III radio burst onset vs. angular separation between the parent flare and s/c footpoints as observed by STA (Λ) and STB (). b) Angular distribution of peak electron intensities normalized to the smallest peak. The pre-event background is subtracted. The letter (F) indicates the s/c that detected the event onset first. The difference in radial distance to the Sun for each s/c is not taken into account; therefore, the values for STB could be 10−20% higher. We note that the first two events (red and blue) are widespread and the third one (green) is a spike event.

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