Magnetic Vortices as Precursor Structures in Flaring Active Regions

Solar flares result from explosive magnetic energy release in the solar atmosphere, often linked to magnetic reconnection. While the underlying physical mechanisms are generally understood, the specific conditions that make an active region (AR) flare at a particular moment remain poorly understood. We aim to investigate the role of magnetic vortices in the flare activity of solar ARs, and to assess whether the presence and evolution of such structures can serve as precursors to major flares. We applied the Integrated Averaged Current Deviation (IACD) method to vector magnetic field data from Helioseismic and Magnetic Imager (HMI)/SHARP for three ARs—AR 11157 (nonflaring), AR 11158, and AR 12673 (both flaring). Time series of IACD values were analyzed using the power spectral density, zeta function scaling, kurtosis, and current helicity to characterize the temporal variability and energy distribution of the vortices. Long-lived magnetic vortices were observed to form and intensify before X-class flare events, followed by abrupt changes and collapse near flare onset. The IACD method isolated these structures more effectively than standard diagnostics, such as magnetograms, current density, or helicity maps. Flaring ARs exhibited flatter power spectra, lower kurtosis, and linear zeta scaling, suggesting more continuous energy accumulation. In contrast, the nonflaring AR displayed steeper spectral slopes, higher kurtosis, and nonlinear zeta scaling, indicative of intermittent and less coherent magnetic activity. Magnetic vortices detected via IACD are promising indicators of flare-productive conditions and may reflect topological changes in the magnetic field. Their temporal evolution provides a potential basis for improving flare forecasting tools.