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Multi-scale structure of the solar wind in the eclipticat 1 AU undergoes significant evolution with the phase of the solar cycle.Wind spacecraft measurements during 1995 to 1998 and ACE spacecraftmeasurements during 1997 to 2005 were used to characterise the evolution ofsmall-scale (~1 min to 2 h) fluctuations in the solar wind speedvsw, magnetic energy density B2, and solar wind ε parameter, in thecontext of large-scale (~1 day to years) variations. The large-scalevariation in ε most resembled large-scale variations in B2. Theprobability density of large fluctuations in ε and B2 both had strongminima during 1995, a familiar signature of solar minimum. GeneralizedStructure Function (GSF) analysis was used to estimate inertial rangescaling exponents aGSF and their evolution throughout 1995 to 2005. Forthe entire data set, the weighted average scaling exponent for small-scalefluctuations in vsw was aGSF=0.284±0.001, a valuecharacteristic of intermittent MHD turbulence (>1/4), whereas the scalingexponents for corresponding fluctuations in B2 and ε wereaGSF=0.395±0.001 and 0.334±0.001, respectively. These valuesare between the range expected for Gaussian fluctuations (1/2) andKolmogorov turbulence (1/3). However, the scaling exponent for ε changed froma Gaussian-Kolmogorov value of 0.373±0.005 during 1997 (end of solarminimum) to an MHD turbulence value of 0.247±0.004 during 2003(recurrent fast streams). Changes in the characteristics of solar windturbulence may be reproducible from one solar cycle to the next

Solar cycle changes in the geo-effectiveness of small-scale solar wind turbulence measured by Wind and ACE at 1 AU