  We analyzed intermittency in the solar wind, as observed on the ecliptic
plane, looking at magnetic field and velocity fluctuations between 0.3 and 1
AU, for both fast and slow wind and for compressive and directional
fluctuations. Our analysis focused on the property that probability
distribution functions of a fluctuating field affected by intermittency become
more and more peaked at smaller and smaller scales. Since the peakedness of a
distribution is measured by its flatness factor we studied the behavior of this
parameter for different scales to estimate the degree of intermittency of our
time series. We confirmed that both magnetic field and velocity fluctuations
are rather intermittent and that compressive magnetic fluctuations are
generally more intermittent than the corresponding velocity fluctuations. In
addition, we observed that compressive fluctuations are always more
intermittent than directional fluctuations and that while slow wind
intermittency does not depend on the radial distance from the sun, fast wind
intermittency of both magnetic field and velocity fluctuations clearly
increases with the heliocentric distance....
