  We study intermittency as a departure from self-similarity of the solar wind
magnetic turbulence and investigate the evolution with the heliocentric
distance and latitude. We use data from the Ulysses spacecraft measured during
two solar minima (1997-1998 and 2007-2008) and one solar maximum (1999-2001).
In particular, by modeling a multifractal spectrum, we revealed the
intermittent character of turbulence in the small-scale fluctuations of the
magnetic field embedded in the slow and fast solar wind. Generally, at small
distances from the Sun, in both the slow and fast solar wind, we observe the
high degree of multifractality (intermittency) that decreases somewhat slowly
with distance and slowly with latitude. The obtained results seem to suggest
that generally intermittency in the solar wind has a solar origin. However, the
fast and slow streams, shocks, and other nonlinear interactions can only be
considered as the drivers of the intermittent turbulence. It seems that
analysis shows that turbulence beyond the ecliptic plane evolves too slowly to
maintain the intermittency with the distance and latitude. Moreover, we confirm
that the multifractality and intermittency are at a lower level than in the
ecliptic, as well as the existence of symmetry with respect to the ecliptic
plane, suggesting that there are similar turbulent properties observed in the
two hemispheres.
