Large-scale structure of the fast solar wind

Details Large-scale structure of the fast solar wind Large-scale structure of the fast solar wind

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgra..11206101b&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue A6, CiteID A06101

Physics

Plasma Physics

10

Solar Physics, Astrophysics, And Astronomy: Coronal Holes, Solar Physics, Astrophysics, And Astronomy: Corona, Space Plasma Physics: General Or Miscellaneous, Interplanetary Physics: Solar Wind Sources, Interplanetary Physics: General Or Miscellaneous

Scientific paper

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 $\odot$ ) 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 $\odot$ ). 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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