The probability distributions of field differences Delta x(tau) = x(t
+ tau) - x(t), where the variable x(t) may denote any solar wind scala
r field or vector field component at time t, have been calculated from
time series of Helios data obtained in 1976 at heliocentric distances
near 0.3 AU. It is found that for comparatively lone time lag tau, ra
nging from a few hours to 1 day, the differences are normally distribu
ted according to a Gaussian. For shorter time lags, of less than ten m
inutes, significant changes in shape are observed. The distributions a
re often spiker and narrower than the equivalent Gaussian distribution
with the same standard deviation, and they are enhanced for large, re
duced for intermediate and enhanced for very small values of Delta x.
This result is in accordance with fluid observations and numerical sim
ulations. Hence statistical properties are dominated at small scale ta
u by large fluctuation amplitudes that are sparsely distributed, which
is direct evidence for spatial intermittency of the fluctuations. Thi
s is in agreement with results from earlier analyses of the structure
functions of Delta x. The non-Gaussian features are differently develo
ped for the various types of fluctuations. The relevance of these obse
rvations to the interpretation and understanding of the nature of sola
r wind magnetohydrodynamic (MHD) turbulence is pointed out, and contac
t is made with existing theoretical concepts of intermittency in fluid
turbulence.