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