Comparison Between Observation and Simulation of Magnetic Field Changes Associated with Flares
Abstract
It has been a long-standing question in solar physics how magnetic field structure changes with eruptive events (e.g., flares and coronal mass ejections). In an effort to understand the physics behind the phenomena, we present the eruption-associated changes in magnetic inclination angle, the horizontal component of magnetic field vectors, the Lorentz force, the magnetic shear angle and the footpoint motion of the flare. The study is mainly based on the three-dimensional MHD simulation of the evolution of the magnetic field in the corona by Yuhong Fan, and compared with some observational data. The results suggest that the field lines at the flaring magnetic polarity inversion line become more horizontal near the surface, that is in agreement with the prediction of Hudson et al. In addition, the footpoints show the de-shearing and diverging motion following the converging motion during the flare.
- Publication:
-
AAS/Solar Physics Division Abstracts #42
- Pub Date:
- May 2011
- Bibcode:
- 2011SPD....42.2220L