Reconnection Theory for Flares (Invited)
Abstract
The principal evidence for reconnection in solar flares comes from observations of flare loops and ribbons during the gradual phase of large-scale events. The motion of these features implies that the rate of reconnection during the gradual phase is relatively fast despite the large value of the magnetic Reynolds number in the corona. This result suggests that current sheets in the lower corona start to dissipate by means of reconnection as soon as they are formed.
- Publication:
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Astronomical Society of the Pacific Conference Series
- Pub Date:
- 1996
- Bibcode:
- 1996ASPC..111..259F
- Keywords:
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- Solar Flares: Magnetic Reconnection