Properties of Magnetohydrodynamic Ibrlmlence in the Solar

The Ulysses mission provides an opportunity to study the cvohrtion of magnetohydrodynarnic (MH D) turbulence in pure high-speed solar wind streams. The absence at high heliocentric latitudes of the strong shears in solar wind velocity generally present near the heliocentric current sheet allows investigation of how fluctuations in the magnetic field and plasma relax and CVOIVC in the radially expanding solar wind. We rcpor~ here results of an analysis of the radial and latitudinal varialion of the turbulence properties of the fluctuations, especially various plasma-field correlations, in high latitude regions. The results constrain current theories of the evolution of MFi D turbulence in the solar wind. Compared to similar observations at 0.3 AU by Hclios, wc find speetra that we similar in having a large frequency band with an ~-1 power spectrum in the outward traveling component of the waves, followed at higher frequencies (larger wave numbers) by a steeper spectrum. Ulysses observations establish that at high latitudes the turbulence is ICSS evolved tharl it is in the ecliptic at the same heliocentric distance and this appears to bc due to the absence of strong velocity shear. Once Ulysses is in the prsl ar coronal hole, properties of the turbulence appear to bc dctcrmincd by the heliocentric distance of the spacecraft rather than by its hclio-latitude.