Elsevier, Journal of Atmospheric and Solar-Terrestrial Physics, 10-11(71), p. 1157-1175
DOI: 10.1016/j.jastp.2008.08.005
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We assess the contributions of various types of solar wind structures (transients, coronal hole high-speed streams (HSS), and slow-speed wind) to hourly average auroral electron power (Pe). The time variation of the solar wind velocity (Vsw) and Pe are determined by HSS, which contribute ∼47% to Pe and Vsw. Transients contribute ∼42% of Pe in solar maxima, and ∼6% in solar minimum. Cross-correlations of Pe with Vsw|B| for negative Bz are significant. Pe exhibits solar rotational periodicities similar to those for Vsw, with strong 7- and 9-day periodicities in 2005–2008 and equinox semiannual periodicities in 1995–1999.