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Solar wind fluctuations, such as magnetic field or velocity, show power lawpower spectra suggestive both of an inertial range of intermittent turbulence(with $\sim -5/3$ exponent) and at lower frequencies, of fluctuations ofcoronal origin (with $\sim -1$ exponent). The ULYSSES spacecraft spent manymonths in the quiet fast solar wind above the Sun's polar coronal holes in ahighly ordered magnetic field. We use statistical analysis methods such as thegeneralized structure function (GSF) and extended self-similarity (ESS) toquantify the scaling of the moments of the probability density function offluctuations in the magnetic field. The GSFs give power law scaling in the``$f^{-1}$'' range of the form $<| y(t+\tau)-y(t)|^{m}>\sim\tau^{\zeta(m)}$,but ESS is required to reveal scaling in the inertial range, which is of theform $<| y(t+\tau)-y(t)|^{m}>\sim [g(\tau)]^{\zeta(m)}$. We find that $g(\tau)$is independent of spacecraft position and$g(\tau)\sim\tau^{-log_{10}(\tilde{\lambda}\tau)}$. The ``$f^{-1}$'' scalingfluctuates with radial spacecraft position. This confirms that, whereas the``$f^{-1}$'' fluctuations are directly influenced by the corona, the inertialrange fluctuations are consistent with locally evolving turbulence, but with an``envelope'' $g(\tau)$, which captures the formation of the quiet fast solarwind.

The signature of evolving turbulence in quiet solar wind as seen by ULYSSES