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tokens: ∼1 month to 27 d, the solar rotation period. An incomplete list of references includes Burlaga Goldstein ( 1984 ), who studied the evolution of plasma flow at 4–5 au and found intermittency in the 5/3 law; they covered a range of 6 months. Marsh Tu ( 1990 ) analysed magnetic field and plasma data from the Helios 1 and Helios 2 spacecrafts between 0.3 and 1 au at the activity minimum of solar cycle 21; they found a −5/3 spectral law, with turbulence better developed in low-speed flows. Espagnet et al. ( 1993 ) computed the power spectra of solar granulation; their energy decreases as a Kolmogorov −5/3 power law in the granulation range (1000–2000 km). Lawrence et al. ( 1995 ) studied ISSN and the 10.7 cm microwave flux; using Fourier and wavelet spectral analysis, they uncovered two regimes of magnetic variability. Cascade (−5/3) behaviour was observed from 2 yr down to 2 d, whereas low dimensional chaotic behaviour was observed at time-scales longer than 8 yr. Abramenko ( 2005 ) worked on images of the photosphere, and extracted the magnetic field of the Sun at times of low flare activity; the study extends over only 60 h. Alexandrova et al. ( 2008 ) computed the power density spectrum using wavelet transforms over a range from 0.1 s to 3 months. McAteer, Gallagher Conlon ( 2010 ) studied turbulence and complexity in order to predict solar flares; using wavelets, these authors found that the PSD of flares is indeed characterized by a −5/3 law. Ashwanden ( 2019 ) recently reviewed models of the solar wind. He noted that, by introducing the reflection of Alfvénic waves, Cranmer van Ballegooijen ( 2005 ) produced ‘a Kolmogorov-like spectrum that does not change dramatically from the photosphere to the solar wind’. The analysis by Plunian et al. ( 2009 ) is the closest to ours and among the most recent ones. As recalled in the Introduction, these authors analysed several kinds of time series of sunspot numbers, concentrations of 14 C in tree rings and 10 Be in polar ice and found two frequency scalings, f − 2/3 when the Sun was active and f − 1 when it was quiescent. These values of exponents are not that expected for Kolmogorov turbulence that should be exactly (within uncertainty) −5/3. Plunian et al. ( 2009 ) suggest that these exponents reflect buoyancy spectra implying values of k − 5/3 and k − 2 for the magnetic energy spectra of the Sun. Plunian et al's ( 2009 ) fig. 3, which displays the PSD of daily and monthly SSN and 10 yr averages of 14 C, ranges from 0.1 to over 10 4 months, shows significant dispersion of the curves, slope changes, and energy peaks at 1 month (27 d) and 10 yr (Schwabe). The −2/3 slope is based on a small range of frequencies (2–20 months). A value of −5/3 (between 1 and 104 months) is not such a bad fit given these uncertainties. But our own results with SSA are much more compelling. 6 CONCLUSION The diverse proxies of solar activity, and in particular solar wind velocity, that have been studied to conclude that