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<p>We explore the oscillations during an M2.3 class solar flare on 2023 December 14, including quasi-periodic pulsations (QPPs) in the light curves and displacement oscillations in the nearby coronal loops, which gives us a chance to investigate whether a physical connection exists between these two phenomena during solar flares. Using the Bayesian-based Markov Chain Monte Carlo (MCMC) and wavelet analysis methods, QPPs are identified in the soft X-ray (SXR), hard X-ray (HXR), and extreme ultraviolet (EUV) light curves. These have a period of around one minute (58 - 72&#xa0;s). High correlations are found between SXR and HXR QPPs indicating that they could be associated with a periodical injection of non-thermal electrons. However, we do not find a time delay between SXR and HXR QPPs at the time resolution of 12&#xa0;s of the data used. Meanwhile, after the flare maximum, two coronal loops rooted in the flare region display expansions and “decayless” oscillations with periods of 3.6&#xa0;min and 8.2&#xa0;min until the flare ending. Our observations suggest that the loop oscillations are most likely standing kink mode waves. The magnetic field strength in the loops is estimated to be 16 G using coronal seismology. We do not find observational evidences showing a physical relation between QPPs and loop oscillations in this event.</p>

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Quasi-Periodic Pulsations and Coronal Loops Oscillations in an M-Class Solar Flare

  • 期刊论文

  • 发表日期：

    2026年5月21日

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  • Yijie Han,
  • Zongjun Ning,
  • Dong Li,
  • Yuzhi Yang,
  • Xiaoyu Tang,
  • Yuxiang Song,
  • Guotianci Xu,
  • Mingbao Gao,
  • Kangyi Li,
  • Yu Huang

摘要

We explore the oscillations during an M2.3 class solar flare on 2023 December 14, including quasi-periodic pulsations (QPPs) in the light curves and displacement oscillations in the nearby coronal loops, which gives us a chance to investigate whether a physical connection exists between these two phenomena during solar flares. Using the Bayesian-based Markov Chain Monte Carlo (MCMC) and wavelet analysis methods, QPPs are identified in the soft X-ray (SXR), hard X-ray (HXR), and extreme ultraviolet (EUV) light curves. These have a period of around one minute (58 - 72 s). High correlations are found between SXR and HXR QPPs indicating that they could be associated with a periodical injection of non-thermal electrons. However, we do not find a time delay between SXR and HXR QPPs at the time resolution of 12 s of the data used. Meanwhile, after the flare maximum, two coronal loops rooted in the flare region display expansions and “decayless” oscillations with periods of 3.6 min and 8.2 min until the flare ending. Our observations suggest that the loop oscillations are most likely standing kink mode waves. The magnetic field strength in the loops is estimated to be 16 G using coronal seismology. We do not find observational evidences showing a physical relation between QPPs and loop oscillations in this event.