UC San Diego
Large-scale structure of the fast solar wind
- Author(s): Bisi, M. M.
- Fallows, R. A.
- Breen, A. R.
- Habbal, S. Rifai
- Jones, R. A.
- et al.
Published Web Locationhttp://www.agu.org/pubs/crossref/2007/2006JA012166.shtml
We present the results of a comprehensive study of the fast solar wind near solar minimum conditions using interplanetary scintillation (IPS) data taken with the EISCAT system in northern Scandinavia, and a recent extremely long baseline observation using both EISCAT and MERLIN systems. The results from IPS observations suggest that the fast wind inside 100 solar radii (R-circle dot) can be represented by a two-mode model in some cases but this distinction is much less clear by in situ distances beyond 1 astronomical unit (215 R-circle dot). Two distinct fast streams are seen in the extremely long baseline IPS observation; comparison of the IPS line of sight with a synoptic map of white light indicates the faster mode overlies the polar crown and the slower fast mode overlies an equatorial extension of the polar coronal hole.
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