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Solar flares are powered by energy stored in the coronal magnetic field, aportion of which is released when the field reconfigures into a lower energystate. Investigation of sunspot magnetic field topology during flare activityis useful to improve our understanding of flaring processes. Here weinvestigate the deviation of the non-linear field configuration from that ofthe linear and potential configurations, and study the free energy availableleading up to and after a flare. The evolution of the magnetic field in NOAAregion 10953 was examined using data from Hinode/SOT-SP, over a period of 12hours leading up to and after a GOES B1.0 flare. Previous work on this regionfound pre- and post-flare changes in photospheric vector magnetic fieldparameters of flux elements outside the primary sunspot. 3D geometry was thusinvestigated using potential, linear force-free, and non-linear force-freefield extrapolations in order to fully understand the evolution of the fieldlines. Traced field line geometrical and footpoint orientation differences showthat the field does not completely relax to a fully potential or linearforce-free state after the flare. Magnetic and free magnetic energies increasesignificantly ~ 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 decreasebut do not return to pre-flare 'quiet' values. The post-flare non-linearforce-free field configuration is closer (but not equal) to that of the linearforce-free field configuration than a potential one. However, the small degreeof similarity suggests that partial Taylor relaxation has occurred over a timescale of ~ 3-4 hours.

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