On the differences in the periodic behaviour of magnetic helicity flux in flaring active regions with and without X-class events

TL;DR

This study analyzes magnetic helicity flux variations in active regions to identify potential precursors of large solar flares, revealing distinct periodic behaviors associated with flaring activity.

Contribution

It introduces a wavelet analysis approach to distinguish periodic patterns in magnetic helicity flux components that correlate with flare occurrence.

Findings

Shorter EM/SH/T periods split after flares in flaring regions.

Longer periods (>10 hrs) remain unchanged before and after flares.

Long-period power (~20 hrs) may serve as a flare precursor.

Abstract

Observational pre-cursors of large solar flares provide a basis for future operational systems for forecasting. Here, we study the evolution of the normalized emergence (EM), shearing (SH) and total (T) magnetic helicity flux components for 14 flaring with at least one X-class flare) and 14 non-flaring ($<$ M5-class flares) active regions (ARs) using the Spaceweather Helioseismic Magnetic Imager Active Region Patches vector magnetic field data. Each of the selected ARs contain a $\delta$-type spot. The three helicity components of these ARs were analyzed using wavelet analysis. Localised peaks of the wavelet power spectrum (WPS) were identified and statistically investigated. We find that: i) the probability density function of the identified WPS peaks for all the EM, SH and T profiles can be fitted with a set of Gaussian functions centered at distinct periods between $\sim$ 3 to 20 hours. ii) There is a noticeable difference in the distribution of periods found in the EM profiles between the flaring and non-flaring ARs, while no significant difference is found in the SH and T profiles. iii) In flaring ARs, the distributions of the shorter EM/SH/T periods ($<$ 10 hrs) split up into two groups after flares, while the longer periods ($>$ 10 hrs) do not change. iv) When the EM periodicity does not contain harmonics, the ARs do not host a large energetic flare. Finally, v) significant power at long periods ($\sim$ 20 hour) in the T and EM components may serve as pre-cursor for large energetic flares.