Theory of coronal streamer formation
Abstract
Conceptually, coronal streamers can form (and disappear) by either of two distinct processes: (1) plasma 'filling' and outward distention of a preexisting closed magnetic structure; and (2) magnetic reconnection, for whatever reason, of an open bipolar field configuration. We argue that the majority of stable-appearing streamers on the Sun at any time are in fact of the latter category - namely, open-field structures undergoing gradual reconnection. Quasi-steady (i.e., 'convectively relaxed') reconnection models may be required to explain the narrow high-density cores exhibited by most streamers out to distances of many solar radii. Some of the observational signatures of reconnection within streamers, which the instrumentation aboard SOHO may be capable of detecting are discussed.
- Publication:
-
NASA STI/Recon Technical Report N
- Pub Date:
- 1992
- Bibcode:
- 1992STIN...9321967K
- Keywords:
-
- Computerized Simulation;
- Magnetic Field Reconnection;
- Magnetohydrodynamic Flow;
- Solar Corona;
- Solar Flares;
- Magnetic Field Configurations;
- Magnetic Flux;
- Magnetic Signatures;
- Plasmas (Physics);
- Solar Physics