EISCAT measurements of the solar wind

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...

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Bibliographic Details
Published in:Annales Geophysicae
Main Authors: A. R. Breen, W. A. Coles, R. R. Grall, M. T. Klinglesmith, J. Markkanen, P. J. Moran, B. Tegid, P. J. S. Williams
Format: Article in Journal/Newspaper
Language:English
Published: Copernicus Publications 1996
Subjects:
Science
Q
Physics
QC1-999
Geophysics. Cosmic physics
QC801-809
EISCAT
Online Access:https://doi.org/10.1007/s00585-996-1235-8
https://doaj.org/article/5de7d6ba0fed4a3aa1bdf59afd7ac37b
Description
Summary: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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