Exploring the relationship between eruptive and non-eruptive solar flares through the periodic behaviour of magnetic helicity flux

Abstract

To better understand the underlying processes and prerequisites for solar activity, it is essential to study the evolution of the lower solar atmospheric magnetic field of solar active regions (ARs) associated with large solar eruptions. Specifically, we aim to explore the relationship between derived quantities and the type of flares produced by the ARs, determining whether they are/are not associated with fast coronal mass ejections (CMEs). In this study, we examined the oscillations of the emergence (EM), shearing (SH), and total (T) components of the magnetic helicity flux in 14 $\delta$-type ARs, building upon the work initiated by Soós et al. (2022). By utilising the measured periods from their wavelet analysis of the three helicity flux components, we sought to further investigate their findings. Initially, it was observed that the periodic components of EM are typically 7 h longer when the flare occurs without a fast CME. Conversely, when the flare is accompanied by a fast CME, the periods of the SH component are generally 6 h longer than those of the EM component. These results support models that differentiate between what is the most dominant physical process of the eruptive and confined flare cases.