arXiv2015
The eruption of the filament with the kink fashion is often regarded as a signature of the kink instability. However, the kink instability threshold for the filament magnetic structure has been not widely understood. Using the H-alpha observation from the New Vacuum Solar Telescope (NVST), we present a partial eruptive filament. In the eruption, a filament thread appeared to split from the middle portion of the filament and to break out in a kinklike fashion. During this period, the left filament material remained below, which erupted without the kinking motion later on. The coronal magnetic field lines associated with the filament are obtained from the nonlinear force-free field (NLFFF) extrapolations using the 12 minutes cadence vector magnetograms of the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamic Observatory (SDO). We studied the extrapolated field lines passing through the magnetic dips that are in good agreement with the observed filament. The field lines are non-uniformly twisted and appear to be made up by two twisted flux ropes winding about each other. One of them has higher twist than the other, and the highly twisted one has its dips aligned with the kinking eruptive thread at the beginning of its eruption. Before the eruption, moreover, the highly twisted flux rope was found to expand with the approximately constant field twist. In addition, the helicity flux maps deduced from the HMI magnetograms show that some helicity is injected into the overlying magnetic arcade, but no significant helicity is injected into the flux ropes. Accordingly, we suggest that the highly twisted flux rope became kink unstable when the instability threshold declined with the expansion of the flux rope.