Yunnan Observatory and others found that the bright front of the coronal mass ejection has a three-layer structure

[ Instrument Network Instrument Research and Development ] Recently, Dr. Mei Zhixing, a member of the solar activity and CME theoretical research group of the Yunnan Observatory of the Chinese Academy of Sciences, and his collaborators, conducted a three-dimensional magnetohydrodynamic (MHD) numerical experiment to study the coronal mass ejection in the solar atmosphere (CME) three-dimensional large-scale structure, related research results were published in the astronomy journal "Astrophysical Journal Letter" (The Astrophysical Journal Letter).
Coronal mass ejections are usually caused by magnetic flux ropes that erupt upward. The white light coronagraph and the extreme ultraviolet (EUV) observations in recent years show that more than 30% of coronal mass ejections have three components, namely, bright nucleus, dark cavity and bright front. Researchers have not reached a consensus on how the explosive magnetic flux rope evolves into a typical CME with three components and its physical nature. Regarding the bright front of CME, early theories believed that the front of CME was a fast mode MHD wave. Later, the CME front was interpreted as the coronal plasma accumulation in front of the explosive magnetic flux rope. Recently, the CME bright front is considered to be the non-wave component of EUV disturbance phenomena.
Researchers carried out high-resolution three-dimensional MHD numerical simulations to study the evolution of the large-scale magnetic structure during the explosion of the magnetic flux rope and its interaction with the background magnetic field. The numerical simulation results show that there are spiral current sheets/boundaries (HCB) around the CME bubble. HCB is a tangential discontinuity in the magnetic structure, which is produced by the interaction between the CME bubble and the ambient magnetic field. Its spiral shape is caused by the Kink process of the magnetic flux rope in the CME bubble.
Based on image synthesis technology, the researchers directly compared the numerical results with the observation images of Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA). In the SDO/AIA composite image, three clear bright fronts are found: a bright fast-mode shock front, a bright HCB, and a bright MFR outer edge, and the three are arranged in order and propagate from the explosion source area.
Regarding the CME outbreak caused by Kink instability, the researchers speculated that HCB may be the bright front of the CME bubble and the non-wave component of the EUV perturbation on the entire surface. This research provides a new theoretical explanation for the formation and evolution mechanism of the CME bright front.
The research work was funded by the National Natural Science Foundation of China and the Yunnan Provincial Applied Basic Research Program.

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