How did the solar wind structure change around the solar maximum? From interplanetary scintillation observation
Observations from the second Ulysses fast latitude scan show that the global structure of solar wind near solar maximum is much more complex than at solar minimum. Soon after solar maximum, Ulysses observed a polar coronal hole (high speed) plasma with magnetic polarity of the new solar cycl...
| Main Authors: | , , , , , , , |
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| Format: | Article |
| Language: | English |
| Published: |
Copernicus Publications
2003-06-01
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| Series: | Annales Geophysicae |
| Online Access: | https://www.ann-geophys.net/21/1257/2003/angeo-21-1257-2003.pdf |