Abstract
Keogram cameras operated at South Pole during 1980 and 1981 have monitored the position, intensity, color, and dynamic behavior of dayside aurora. The position of the midday aurora for very quiet magnetic conditions is some 5° further poleward than was previously recognized. The average energy of dayside electron precipitation (∼100 eV) does not change as magnetic activity increases. Rapid latitudinal movements of discrete dayside aurora structures and pulsating structures with Pc 5 periodicities are regularly observed and have no obvious explanation in terms of interplanetary field conditions.
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