Abstract
EISCAT observations of interplanetary scintillation have been used to measure the velocity of the solar wind at distances between 15 and 130 solar radii (R). The results show that away from transients and interaction regions the solar wind consists of two distinct components - a fast stream with a velocity of ∼700–800 km/s and a slow stream at ∼300–400 km/s. Both the fast and slow streams finish their acceleration much closer to the Sun than expected, with the acceleration much closer to the Sun than expected, with the acceleration of the fast high latitude solar wind being effectively complete inside 10 R. The flow vector of the solar wind is normally purely radial to the Sun, although one set of observations suggests a small but significant deviation from radial flow.
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