Modelling Observable Differences in Flare Loop Evolution Due to Current Sheet Structure
Abstract
Solar flares are the most energetic event in the solar system. These events are triggered when magnetic reconnection occurs in a current sheet in the corona above a magnetic active region. Energy release in a solar flare is dictated by the retraction of magnetic flux post-reconnection. The characteristics of the magnetic field are expected to affect this process. Different models for reconnection suggest different structures for the magnetic field. Models invoking Petschek-type reconnection use a uniform field. Others invoke a field bounded by two Y-points, such that the field strength is maximum in the middle. Still other models, such as a collapsing trap model, require that the field strength peak near or at the edge of the current sheet. We use a thin flux tube (TFT) framework to study the effects of the field structure on a bundle of retracting flux. Using a constant magnetic field, this approach returns Petschek-type results. Here, we have modified this framework to use a non-uniform magnetic field. With this, we can now compare the expected evolution of flux bundles using different magnetic field configurations. We find that different magnetic field structures lead to a distinct difference in the evolution of a flux bundle.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2019
- Bibcode:
- 2019AGUFMSH13D3420U
- Keywords:
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- 7519 Flares;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7554 X-rays;
- gamma rays;
- and neutrinos;
- SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7845 Particle acceleration;
- SPACE PLASMA PHYSICS;
- 7974 Solar effects;
- SPACE WEATHER