Data obtained during the IMS with a ground‐based chain of meridian photometers which measured the Hβ and OI 5577‐A emissions have been analyzed quantitatively to yield the mean distributions of proton and electron aurora in geomagnetic latitude and time as functions of magnetic activity. The total energy inputs from electron and proton precipitation around the nightside auroral oval are estimated as functions of AE from the 5577‐A and Hβ intensity data. Average latitude profiles for the two emissions are given as a function of AE for the four night time sectors between 1800 and 0600 local magnetic time. In agreement with previous studies it is found that the average energy flux due to protons is an order of magnitude less than that due to electrons under disturbed conditions although under very quiet conditions the two are comparable. Finally, the Hβ observations have been fitted to a quantitative empirical model giving Hβ intensity distributions as a function of AE. The peak values of Hβ intensity increase linearly with AE for all magnetic time sectors.
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Creutzberg et al. (1988) studied this question.