Coronal models
Abstract
Coronal holes are regions that appear dark in EUV and X-ray emission on the solar disk. The general qualitative picture of these regions, that they are magnetically open and are the origin of the fast solar wind, has strong observational support. However, many details of this picture are unclear, such as: What happens at the edges of coronal holes? Are the edges primarily steady structures, or are they opening and closing? Is the open magnetic flux at 1 AU well-accounted for by the magnetic flux emanating from coronal holes? What do disagreements in coronal hole boundaries from different emission lines tell us about there structure? In this talk we will discuss how these questions can be approached from a theoretical and modeling perspective.
- Publication:
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Solar Heliospheric and INterplanetary Environment (SHINE 2013)
- Pub Date:
- June 2013
- Bibcode:
- 2013shin.confE..20L