Evidence for Partial Taylor Relaxation from Changes in Magnetic Geometry and Energy during a Solar Flare

Abstract

Solar flares are powered by energy stored in the coronal magnetic field, a portion of which is released when the field reconfigures into a lower energy state. Investigation of sunspot magnetic field topology during flare activity is useful to improve our understanding of flaring processes. Here we investigate the deviation of the non-linear field configuration from that of the linear and potential configurations, and study the free energy available leading up to and after a flare. The evolution of the magnetic field in NOAA region 10953 was examined using data from Hinode/SOT-SP, over a period of 12 hours leading up to and after a GOES B1.0 flare. Previous work on this region found pre- and post-flare changes in photospheric vector magnetic field parameters of flux elements outside the primary sunspot. 3D geometry was thus investigated using potential, linear force-free, and non-linear force-free field extrapolations in order to fully understand the evolution of the field lines. Traced field line geometrical and footpoint orientation differences show that the field does not completely relax to a fully potential or linear force-free state after the flare. Magnetic and free magnetic energies increase significantly ~ 6.5-2.5 hours before the flare by ~ 10^31 erg. After the flare, the non-linear force-free magnetic energy and free magnetic energies decrease but do not return to pre-flare 'quiet' values. The post-flare non-linear force-free field configuration is closer (but not equal) to that of the linear force-free field configuration than a potential one. However, the small degree of similarity suggests that partial Taylor relaxation has occurred over a time scale of ~ 3-4 hours.

Accepted for Publication in Astronomy & Astrophysics. 11 pages, 11 figures

References in corpus (9)

• The Solar Optical Telescope for the Hinode Mission: An Overview
• Optimization code with weighting function for the reconstruction of coronal magnetic fields
• Preprocessing of vector magnetograph data for a non-linear force-free magnetic field reconstruction
• Comparing magnetic field extrapolations with measurements of magnetic loops
• Free Magnetic Energy in Solar Active Regions above the Minimum-Energy Relaxed State
• Observational Test of Coronal Magnetic Field Models I. Comparison with Potential Field Model
• Nonlinear force-free models for the solar corona I. Two active regions with very different structure
• First nonlinear force-free field extrapolations of SOLIS/VSM data
• Comparison of Nonlinear Force-free Field and Potential Field in the Quiet Sun

Cited by in corpus (3)

• Solar Force-free Magnetic Fields
• Flaring Rates and the Evolution of Sunspot Group McIntosh Classifications
• Three-dimensional magnetic reconnection in a collapsing coronal loop system