In a recent study published in The Astrophysical Journal, HU Jialiang and Prof. LIN Jun from Yunnan Observatories (YNAO) of the Chinese Academy of Sciences, and the collaborators, proposed a new mechanism for the generation of large-scale quasiperiodic fast-propagating (QFP) magnetoacoustic waves on both sides of coronal mass ejection (CME).

The magnetized solar atmosphere, a highly structured medium, supports various types of wave generation and propagation. The quasi-periodic wave trains in the corona (QFP waves) are coronal disturbance phenomena observed by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO). These wave fronts, interpreted as fast-mode magnetoacoustic waves, consist of continuous, narrow arc structures, capable of rapid propagation at speeds up to 1416 km/s.

Based on current observational constraints, the origin of QFP waves remains unclear. Numerous mechanisms have been proposed to explain the relationship between CMEs or flares and QFP waves, but a definitive conclusion has not yet to be reached. This study sheds new light on the origin of QFP waves.

Numerical simulations revealed that magnetic flux rope containing helical magnetic structures exhibits waveguide properties. When surrounding coronal magnetic structures destabilize, oscillations occur within the flux rope. Since the magnetic flux rope is not a perfect waveguide, the internal oscillations propagate to the boundaries and partially leak into the surrounding corona, forming the observed QFP waves.

To gain a deeper understanding of the origin of QFP waves, the researchers analyzed the propagation characteristics of disturbances by calculating velocity divergence at different times, yielding results consistent with observations.

Furthermore, synthetic images based on simulated data in extreme ultraviolet and white light highly reproduced actual observational results. This consistency of the simulation result with observation demonstrated that the leakage of internal disturbances from the flux rope, acting as a waveguide, forms a multi-wavefront structure and represents a reasonable mechanism for the generation of QFP waves.

The numerical computation in this study was carried out on the computing facilities of the Computational Solar Physics Laboratory of YNAO.