Effect of Solar Flares on Decayless Kink Oscillations in Nearby Coronal Loops

We present a statistical study of 130 solar flares (B to X class) that lack soft X-ray quasiperiodic pulsations and show no kink oscillations of nearby coronal loops visible in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 171 Å images. The aim is to investigate whether decayless kink oscillations of coronal loops respond to nearby flaring activity. Using the Fractional Anisotropy-based Video Motion Magnification technique, we detected low-amplitude decayless oscillations in all 130 loops before, during, and after each flare, confirming their ubiquitous nature. Oscillation periods are found to range from 122 to 268 s, and the projected displacement amplitudes are 0.023–0.111 Mm. No amplitude–period correlation is found. For each event, we estimated the amplitude before, during, and after the flare. Across all flare classes, the average amplitude remains unchanged. However, in some specific cases, the oscillation amplitude may exhibit minor changes. For B-, C-, and M-class flares, the fraction of events with an amplitude change exceeding 10% is approximately 23%, 41%, and 36%, respectively. In M-class flares, such minor amplitude increases occur 4 times more often than decreases; in X-class flares (only six events), decreases dominate by a factor of 3. The fraction of events that exhibit an increase in the amplitude of more than 20% appears to be highest when the loop center is located at a distance of 100–120 Mm from the flare site, reaching 33% (6 out of 18 events). Overall, the amplitude of decayless kink oscillations does not undergo a major change in response to nearby flares, especially for less powerful classes, suggesting that flare-related processes such as blast waves and reconnection inflows have little effect on the energy supply to oscillating loops.