On May 1, The Astrophysical Journal Letter published the latest work conducted by Dr. ZHOU Xinping from Yunnan Observatories of the Chinese Academy of Sciences and his co-authors, on the broad Extreme-Ultraviolet (EUV) wave train. Their study result implies that the broad EUV wave train, including multiple wave fronts, should be driven by some nonlinear energy release processes in the accompanying flare.

Generally, the single, diffused, bright disturbance is always thought to be a fast-mode piston shock and bow shock driven by a coronal mass ejection's (CME's)  expansion. Although this scenario can explain many observational features of the large-scale coronal waves, it is hard to distinguish whether a particular EUV wave is driven by a CME or ignited by a flare because the CME acceleration phase generally synchronizes with the flare’s impulsive phase.

Using the high spatio-temporal imaging observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA), ZHOU Xinping and his co-authors found that a broad EUV wave train composed multiple large-scale wave fronts. This wave train is hard to be explained by using the CME lateral expansion theory. They found that the physical parameters of the wave train, such as speed, amplitude, and energy flux were consistent with the classical large-scale EUV wave.

At the same time, their analysis result shows that the CME acceleration phase’s beginning time was behind the first wave front’s appearance. In contrast, the beginning time of the wave train was slightly behind the onset of the accompanying flare. Combined with the above observational fact and the common period between the accompanying flare and wave train, ZHOU Xinping and his co-authors proposed that the flare rather than the CME triggered the wave train.

This study result might provide a reliable case for supporting the flare-driven mechanism of the EUV waves. In addition, this study also provides the first evidence of the interference effect of EUV waves, suggesting the true wave nature of the observed disturbance.

Contact:
SHEN Yuandeng
Yunnan Observatories, CAS
E-mail: ydshen@ynao.ac.cn