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Ann. Geophys., 14, 1235-1245, 1996
www.ann-geophys.net/14/1235/1996/
© European Geosciences Union 1996
EISCAT measurements of the solar wind
A. R. Breen1, W. A. Coles2, R. R. Grall2, M. T. Klinglesmith2, J. Markkanen3, P. J. Moran1, B. Tegid1, and P. J. S. Williams1
1Adran Ffiseg, Prifysgol Cymru, Aberystwyth SY23 4LU, Cymru/Wales, EU
2Department of Electrical and Computer Engineering, University of California, San Diego, USA
3EISCAT, Sodankylä SF-99600, Suomi/Finland, EU
Abstract. EISCAT observations of interplanetary
scintillation have been used to measure the velocity of the solar wind at
distances between 15 and 130 R⊙ (solar radii) from the Sun.
The results show that the solar wind consists of two distinct components, a fast
stream with a velocity of ~800 km s–1 and a slow stream at ~400 km s–1.
The fast stream appears to reach its final velocity much closer to the Sun than
expected. The results presented here suggest that this is also true for the slow
solar wind. Away from interaction regions the flow vector of the solar wind is
purely radial to the Sun. Observations have been made of fast wind/slow wind
interactions which show enhanced levels of scintillation in compression regions.
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