Solar wind structure sources and periodicities of auroral electron power over three solar cycles

Abstract 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 ( P e ). The time variation of the solar wind velocity ( V sw ) and P e are determined by HSS, which contribute ∼47% to P e and V sw . Transients contribute ∼42% of P e in solar maxima, and ∼6% in solar minimum. Cross-correlations of P e with V sw |B| for negative B z are significant. P e exhibits solar rotational periodicities similar to those for V sw , with strong 7- and 9-day periodicities in 2005–2008 and equinox semiannual periodicities in 1995–1999.

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