The heliographic latitude-longitude structure of high speed solar wind streams observed prior to the maximum of solar cycle 20 has been studied with a multi-spacecraft comparison. Plasma and magnetic field data obtained near the earth by Explorers 34 and 35 during mid-1967 were mapped radially inward to the location of Mariner 5, which was making simultaneous measurements at lower heliographic latitudes. For latitude separations less than 3.5¿, cross-correlations of the Explorer-Mariner velocities showed only the previously reported systematic increase in velocity with latitude. However, for latitude separations ranging from 3.5¿ to 6.2¿, significant differences in the high speed stream structure of up to 250 km/s were seen. For these stream structures, the multi-spacecraft observations made possible the separation of spatial from temporal variations with little ambiguity. Within one interval, the higher-latitude Explorers saw a single, broad stream while the lower-latitude Mariner saw a series of three relatively narrow streams. Within a second interval, a single higher speed stream was observed at both locations which was sloped at an angle of 70¿--80¿ from solar-south direction. These stream structures, which were also seen by Pioneers 6 and 7, imply the existence of large, temporary, local north-south velocity gradients, or wind shears, ranging up to 60 km/s/deg. The latitude separations found for these structural differences were the smallest yet observed in spacecraft data and hence involved shorter corotation delays than those of any previous study. The multi-spacecraft comparisons also led to the identification of several intervals of time when individual high speed streams shifted substantially in either longitude and/or amplitude on a time scale of one solar rotation. Possible flare-related disturbances were found to be too small to account for these large observed changes.