The magnetic field intermittent structures in fast-solar-wind turbulence are studied by using measurements from the WIND spacecraft and are,by the help of the technique described by Smith (1973),identified as being mostly rotational discontinuities (RDs)and rarely tangential discontinuities (TDs).Only the TD-associated current sheets are found to be accompanied with local heating of the solar wind protons,but statistically their heating effect is not prominent.While for RDs,our results do not reveal significant heating.The relation between the intermittency and the anisotropy of the turbulent power spectra is also studied by applying the wavelet technique to the magnetic field and flow velocity data of the solar wind.It is found that when the intermittency is removed from the turbulence,the spectral indices of the power spectra of the field and velocity turn out to be independent of the angle between the direction of the local scale-dependent background magnetic field and the heliocentric radial direction.The spectral index is found to be-1.63±0.02 for magnetic field fluctuations and-1.56±0.02 for velocity fluctuations.These results may suggest that the anisotropy of solar wind power spectra in the inertial range could result from intermittency.As a consequence,a new concept is proposed here that in the inertial domain adjacent to the dissipation range there may be a sub-range abundant in intermittency,which is responsible for the spectral anisotropy.Since the spectral anisotropy was previously explained as evidence for the presence of a "critical balance" type turbulent cascade,and also for the existence of kinetic Alfven waves,this new finding may stimulate fresh thoughts on how to analyze and interpret solar wind turbulence.