Large-scale structure of the fast solar wind

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...

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Bibliographic Details
Published in:Journal of Geophysical Research: Space Physics
Main Authors: Bisi, M. M., Fallows, R. A., Breen, A. R., Habbal, S. Rifai, Jones, R. A.
Format: Article in Journal/Newspaper
Language:English
Published: eScholarship, University of California 2007
Subjects:
EISCAT
MERLIN
Interplanetary Scintillation (IPS)
Solar Wind
Bi-modal fast wind
Tri-modal model
Ulysses SWOOPS
SOHO LASCO
SOHO EIT
Yohkoh SXT
Mauna Loa MkIII
Online Access:http://www.escholarship.org/uc/item/56s54973
Description
Summary: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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