Speaker
Description
While asymmetric eruptions and nonradial propagation of solar filaments are typically attributed to inhomogeneous overlying magnetic fields, the role of the filaments’ intrinsic asymmetry remains underexplored. In this work, we analyze the evolution of an intermediate-type filament from its activation and asymmetric eruption to its propagation alongside an associated coronal mass ejection (CME). Contrary to expectations, magnetic cancellation and a lower critical height for torus instability were identified at the filament's confined leg. Intermittent bursts originating from the magnetic cancellation region supplied hot plasma to the filament and drove unidirectional flows toward the eruptive leg. Alongside these bursts, H$\alpha$ Doppler images clearly revealed enhanced filament asymmetry: prior to eruption, the eruptive leg exhibited a larger cross-section, more dynamic flows, and persistent blueshift. Durig the propagation, the erupting filament initially had a larger inclination angle than the CME, which was consistent with the asymmetric eruption behavior; the filament's inclination gradually aligned with that of the CME as the event progressed. Finally, we discuss the combined effects of the overlying magnetic field and the filament's intrinsic magnetic field on both the eruption and subsequent propagation.
