Articles | Volume 14, issue 12
Ann. Geophys., 14, 1235–1245, 1996
https://doi.org/10.1007/s00585-996-1235-8

Special issue: VIIIe EISCAT

Ann. Geophys., 14, 1235–1245, 1996
https://doi.org/10.1007/s00585-996-1235-8

  31 Dec 1996

31 Dec 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 A. R. Breen et al.
  • 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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