EXPLORATION OF THE COMPRESSIBILITY, VORTICITY AND OTHER TURBULENCE PROPERTIES OF THE SOLAR WIND USING MULTIPLE SPACECRAFT AN EXPLORATORY STUDY OF TURBULENCE IN THE SOLAR WIND USING SPATIAL DERIVATIVES (COMPRESSIBILITY AND VORTICITY) DERIVED FROM THE IN-SITU OBSERVATIONS OF THE ELECTRON PLASMA. THE DIRECT COMPUTATION OF SPATIAL DERIVATIVES ALLOWS FOR DIRECT SOLUTIONS OF THE EQUATIONS REPRESENTING SEVERAL VARIABLES OF INTEREST TO TURBULENCE SUCH AS ENSTROPY, THE TAYLOR MICROSCALE, AND THE KINEMATIC VISCOSITY. THESE ARE MADE WITH THE SAME 4 SEC TIME RESOLUTION USED TO COMPUTE THE COMPRESSION AND VORTICITY. THE PROPOSED STUDY INVOLVES ANALYSIS OF THE LIMITATIONS OF USING ELECTRON DATA TO REPRESENT THE BASIC SOLAR WIND PARAMETERS (DENSITY, VELOCITY, ETC), ERRORS INVOLVED IN COMPUTING SPATIAL DERIVATIVES OF THE VELOCITY, UNDERSTANDING WHAT IS SEEN IN MEASURED COMPRESSION AND VORTICITY PLOTS, AND THE APPLICATION SPATIALLY DERIVED PARAMETERS TO SOLAR WIND TURBULENCE. THE STUDY WILL LOOK AT DIFFERENCES IN THE VORTICITY IN FAST AND SLOW SOLAR WIND AND HOW THESE RELATE TO POSSIBLE DIFFERENCES IN THE DISSIPATION MECHANISMS, THE POSSIBILITY OF COUPLING MAGNETIC TURBULENCE TO THE ELECTRONS THROUGH THE STRAHL, AND THE USE OF ENSTROPHY SPECTRA TO EXPLORE REGIONS OF DISSIPATION AND INTERMITTENCY.