Space Climate
Open Access

Fig. 5.


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The sunspot number (top panel) together with three-rotation averages of the αα geomagnetic index in all-solar-wind, and in CME-associated flows, corotating streams, and slow solar wind separately (note changes in vertical scale). Arrows indicate temporary depressions in αα around solar maximum related to the “Gnevyshev Gap”. Note that the lowest values of αα during this period, in the solar minimum following cycle 23, are evident in all the solar wind flow types. The all-solar-wind results are overplotted on those for streams, showing that average values of αα tend to track those in streams, as previously noted by Richardson et al. (2001).

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