Observational Diagnostics of Reconnection in Solar Flares
Abstract
Magnetic reconnection is believed to be the prime means of releasing magnetic energy in a solar flare. The process of reconnection occurs on spatial scales significantly smaller than the best observationally resolvable scales.Consequently, we must rely on observational signatures which, indirectly, imply the presence of magnetic reconfiguration in the form of reconnection. Recent, high-resolution, multi-wavelength flare observations are allowing us to use the observed dynamical behavior to probe the connection between the small-scale localized trigger and the large-scale coronal field which ultimately participates in the solar flare. We will discuss some new results which indicate strong evidence for the presence of 3D coronal reconnection and the role it plays in the dynamics of the flare plasma.
- Publication:
-
AGU Spring Meeting Abstracts
- Pub Date:
- May 2001
- Bibcode:
- 2001AGUSM..SM22A10A
- Keywords:
-
- 7500 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7519 Flares;
- 7524 Magnetic fields