  Filament eruption is a common phenomenon in solar activity, but the
triggering mechanism is not well understood. We focus our study on a filament
eruption located in a complex nest of three active regions close to a coronal
hole. The filament eruption is observed at multiple wavelengths: by the GONG,
the STEREO, the SUTRI, and the AIA and Helioseismic and Magnetic Imager (HMI)
on board the SDO. Thanks to high temporal-resolution observations, we were able
to analyze the evolution of the fine structure of the filament in detail. The
filament changes direction during the eruption, which is followed by a halo
coronal mass ejection detected by the LASCO on board the SOHO. A Type III radio
burst was also registered at the time of the eruption. To investigate the
process of the eruption, we analyzed the magnetic topology of the filament
region adopting a nonlinear force-free-field (NLFFF) extrapolation method and
the polytropic global magnetohydrodynamic (MHD) modeling. We modeled the
filament by embeddingatwisted fluxropewiththe regularized Biot-Savart Laws
(RBSL) method in the ambient magnetic f ield. The extrapolation results show
that magnetic reconnection occurs in a fan-spine configuration resulting in a
circular flare ribbon. The global modeling of the corona demonstrates that
there was an interaction between the filament and open field lines, causing a
deflection of the filament in the direction of the observed CME eruption and
dimming area. The modeling supports the following scenario: magnetic
reconnection not only occurs with the filament itself (the flux rope) but also
with the background magnetic field lines and open field lines of the coronal
hole located to the east of the flux rope. This multiwavelength analysis
indicates that the filament undergoes multiple magnetic reconnections on small
and large scales with a drifting of the flux rope.
