Research into the Magnetic Configuration of Eruptive Filaments with a High-class Flare

Abstract Filament eruptions are the source of coronal mass ejections, and these phenomena are likely to pose a serious threat to space weather safety. The magnetic structures that carry the filament material are considered the core structures of the eruption, and they may drive the eruption through magnetohydrodynamic instabilities and magnetic reconnection. In this study, we successfully performed three-dimensional magnetic field reconstruction of the corona for 16 filament eruption events associated with strong flares (at least M-class) between 2011 and 2022, and all the magnetic structures can be strictly matched with the EUV observational morphology of the filaments. We further calculated and analyzed the parameters used to characterize the MHD instabilities and magnetic reconnection of the magnetic structures. The kink instability parameter indicated that almost all events exhibited twisted features of a magnetic flux rope before the eruption, while the torus instability parameter was generally low. On the other hand, in the map of the Q -value distribution, which describe whether the connectivity of the magnetic structure is prone to change, we found that more than 60% of the magnetic ropes exhibited obvious reconnection features. Combining this with evolutionary diagrams of the positions of the filament material, we suggest that, in the environment of strong flares, magnetic reconnection plays a more important role in triggering filament eruption events than torus instability.