The Acceleration Process of a Solar Quiescent Filament in the Inner Corona

Coronal mass ejections (CMEs) are frequently associated with filament eruptions. Theoretical studies propose that both magnetic reconnection and ideal magnetohydrodynamic instability of magnetic flux ropes can convert coronal magnetic energy into the filament/CME kinetic energy. Numerical simulation...

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Veröffentlicht in:	Astrophysical journal. Letters 2018-04, Vol.857 (2), p.L21
Hauptverfasser:	Song, H. Q., Chen, Y., Qiu, J., Chen, C. X., Zhang, J., Cheng, X., Shen, Y. D., Zheng, R. S.
Format:	Artikel
Sprache:	eng
Schlagworte:	Acceleration Computational fluid dynamics Computer simulation Corona Coronal mass ejection Eruptions Fluctuations Fluid flow instabilities Instability Kinetic energy Magnetic flux Magnetic reconnection Magnetohydrodynamic stability Magnetohydrodynamics Numerical simulations Stability Stability analysis Sun: coronal mass ejections (CMEs) Sun: flares
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