Abstract
Multi-site measurements of interplanetary scintillation (IPS) can provide information on solar wind velocity at any heliolatitude or longitude and over a wide range of heliocentric distances, with the coverage limited only by the availability of suitable radio sources and the geometry of the observing system. The EISCAT facility has been used to make IPS measurements every summer from 1989 to the present day. In this paper we discuss results from solar minimum in 1996, through the rising phase of cycle 23 to the spring of 2000. We discuss the changes in the large-scale structure of the solar wind seen in the EISCAT IPS data and compare them with results from the Nagoya IPS system and with structures seen in coronal white-light intensity.
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