Abstract
N are systematically high with respect to this prior expression. (3) Our estimates for the speed at which the irregularities move with respect to the antennas, and in the radial direction from the Sun, are in the range of 190{340 km s 1 for heliocentric distances of 16{26 R. These values are in good agreement with observational estimates of the solar wind flow speed in this part of space based on coronagraph observations. The speeds are lower than the sum of the estimated solar wind flow speed and the local Alfv en speed. The potential signicance of this result is discussed.
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