Interplanetary scintillation measurements of the solar wind during Whole Sun Month: Comparisons with coronal and in situ observations

Two-site observations of interplanetary scintillation using the EISCAT faci lity can provide measurements of solar wind velocity at any point in the he liosphere between 15 and 120 solar radii (R). Ln this paper we discuss a se ries of observations made as part of the Whole Sun Month campaign (August 1 0 to September 8, 1996) and compare the results with coronal data and in-si tu measurements made during the campaign. The results of the comparison rev ealed extremely good agreement between solar wind speeds measured by IFS at 16-73 R and in situ measurements at 213 R and beyond, both in the general morphology of the solar wind and in the absolute velocities observed. These results confirm that structures in the solar wind, originating in the coro na, preserve their form out to 910 R or more. Observations of fast solar wi nd were always associated with coronal holes and slow wind with the bright corona. Velocities intermediate between normal fast and slow flow speeds ar e associated with interaction regions between fast and slow flow and are al so found above the boundaries of coronal holes.