Coronal Evolution and Heating by Magnetic Reconnection in Closely Packed Flux Tubes
Abstract
It is now widely accepted that the solar corona is heated to temperatures of more than 106K by a magnetic mechanism, with energy supplied by motions of the photospheric footpoints of the coronal magnetic field. One approach to heating by reconnection has been developed by Parker (1972, 1982, 1983). While Parker suggests that the field will reconnect and release heat, the ultimate state of the field and the amount of energy released are yet to be determined. The author's aim is to develop an alternative approach to answer these questions, using some recent developments in coronal heating theory which is outlined here.
- Publication:
-
Solar Maximum Analysis
- Pub Date:
- 1987
- Bibcode:
- 1987sman.work..173B