  Solar filament eruptions are often characterized by stepwise evolution due to
the involvement of multiple mechanisms, such as magnetohydrodynamic
instabilities and magnetic reconnection. In this article, we investigated a
confined filament eruption with a distinct two-stage evolution by using the
imaging and spectroscopic observations from the Interface Region Imaging
Spectrograph (IRIS) and the Solar Dynamics Observatory (SDO). The eruption
originated from a kinked filament thread that separated from an active region
filament. In the first stage, the filament thread rose slowly and was
obstructed due to flux pile-up in its front. This obstruction brought the
filament thread into reconnection with a nearby loop-like structure, which
enlarged the flux rope and changed its connectivity through the foot-point
migration. The newly formed flux rope became more kink unstable and drove the
rapid eruption in the second stage. It ascended into the upper atmosphere and
initiated the reconnection with the overlying field. Finally, the flux rope was
totally disintegrated, producing several solar jets along the overlying field.
These observations demonstrate that the external reconnection between the flux
rope and overlying field can destroy the flux rope, thus playing a crucial role
in confining the solar eruptions.
