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We present the results of a study of solar wind velocity and magnetic fieldcorrelation lengths over the last 35 years. The correlation length of themagnetic field magnitude lambda(|B|) increases on average by a factor of two atsolar maxima compared to solar minima. The correlation lengths of thecomponents of the magnetic field lambda(Bxyz) and of the velocity lambda(Vyz)do not show this change and have similar values, indicating a continualturbulent correlation length of around 1.4 x 10^6 km. We conclude that a linearrelation between lambda(|B|), VB^2 and Kp suggests that the former is relatedto the total magnetic energy in the solar wind and an estimate of the averagesize of geo-effective structures which is in turn proportional to VB^2. Bylooking at the distribution of daily correlation lengths we show that the solarminimum values of lambda(|B|) correspond to the turbulent outer scale. A tailof larger lambda(|B|) values is present at solar maximum, causing the increasein mean value.

The Variation of Solar Wind Correlation Lengths Over Three Solar Cycles