Associating the solar wind measured by Ulysses with its source at the sun

Radio occultation, ultraviolet, and white-light measurements have expanded our knowledge of the morphology of density and velocity in polar coronal ho les, and made it possible to carry out the first systematic comparisons bet ween the Ulysses solar wind measurements and quantitative white-light obser vations of the solar corona. This paper summarizes the rationale and salien t features of this new approach which has been used to relate the solar win d observed by Ulysses in 1993-1995 to the inner corona. The statistical cha racteristics (average, standard deviation, and autocorrelation function) of the Ulysses density measurements of the fast wind are found to be mirrored in those of polarized brightness measurements of path-integrated density m ade by the High Altitude Observatory (HAO) Mauna Loa K-coronagraph at 1.15 R-circle dot. These results reinforce the conclusions from comparisons betw een measurements of the outer and inner corona. They show that the polar co ronal hole extends radially into the solar wind, and that sources of the fa st wind are not limited to coronal holes.