Prevalence of non-stationarity in quasi-periodic pulsations (QPPs) associated with M- and X-class solar flares

Abstract

ABSTRACT Quasi-periodic pulsations (QPPs) are frequently observed in solar and stellar flare emission, with recent studies suggesting that an increasing instantaneous period is a common characteristic of QPPs. Determining the prevalence of non-stationarity in QPPs contributes to a better understanding of which mechanism(s) is (are) responsible in QPP generation. We obtain the rate of period evolution from QPPs in 98 M- and X-class flares from Solar Cycle 24 with average periods between 8 and 130 s and investigate the prevalence of QPP non-stationarity. We also investigate whether the presence of a coronal mass ejection (CME) impacts the period evolution of QPPs. We analyse soft X-ray light curves obtained from GOES’ X-ray sensor (XRS) and assess the dominant periods in the impulsive and decay phases of the flares using the fast Fourier transform. We relate the rate of period evolution to flare duration, peak flare energy, and average QPP period. We find evidence of non-stationarity in 81 per cent of the flares assessed, with most QPPs exhibiting a period evolution of ≤10 s between the impulsive and decay phases, of which 66 per cent exhibited an apparent period growth and 14 per cent showed an apparent period shrinkage. We find a positive correlation between the absolute magnitude of period evolution and the duration of the flare and no correlation between the period evolution of the QPPs and flare energy or CME presence. Furthermore, we conclude that non-stationarity is common in solar QPPs and must be accounted for in flare analysis.