Magnetic Flux Change and Cancellation Associated with X-class and M-class Flares

TL;DR

This study analyzes magnetic flux changes during solar flares, revealing that flux decreases and cancellations are common, especially in X-class flares, supporting models of collapsing magnetic loops and highlighting the role of field complexity.

Contribution

It provides a statistical analysis of magnetic flux changes during flares using feature tracking, emphasizing flux cancellation and its relation to flare magnitude and location.

Findings

More flux decreases than increases during flares.

Flux cancellation correlates with flare strength, especially in X-class flares.

Field complexity near the polarity inversion line influences flux cancellation.

Abstract

We perform a statistical study of permanent changes in longitudinal fields associated with solar flares by tracking magnetic features. The YAFTA feature tracking algorithm is applied to GONG++ one-minute magnetograms for 77 X-class and M-class flares to analyze the evolution and interaction of the magnetic features and to estimate the amount of canceled magnetic flux. We find that significantly more magnetic flux decreases than increases occurred during the flares, consistent with a model of collapsing loop structure for flares. Correlations between both total (unsigned) and net (signed) flux changes and the GOES peak X-ray flux are dominated by X-class flares at limb locations. The flux changes were accompanied in most cases by significant cancellation, most of which occurred during the flares. We find that the field strength and complexity near the polarity inversion line are approximately equally important in the flux cancellation processes that accompany the flares. We do not find a correlation between the flux cancellation events and the stepwise changes in the magnetic flux in the region.