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We present the formation and eruption of a sigmoidal filament driven byrotating network magnetic fields (RNFs) near the center of the solar disk,which was observed by the one-meter aperture New Vacuum Solar Telescope (NVST)at Fuxian Solar Observatory (FSO) on 2018 July 12. Counterclockwise RNFs twisttwo small-scale filaments at their northeastern foot-point region, giving arotation of nearly 200 degree within about 140 minutes. The motion of the RNFhas a tendency to accelerate at first and then decelerate obviously, as theaverage rotation speed increased from 10 to 150 ,and then slowed down to 50 .Coalescence then occurs between filaments F1 and F2. Meanwhile the finestructures in the southwestern region of the filament was involved in anotherinteraction of coalescence. The subsequent EUV brightening due to plasmaheating is observed in the two interaction regions. These interactingstructures, including F1, F2 and the fine structures in the southwesternregion, eventually evolve into a larger-scale sigmoidal filament twisted in thesame direction as the RNFs gave. The twist of the sigmoidal filament hasexceeded 4{\pi} and the filament erupted finally. The motion of the sigmoidalfilament keeps uniform until a nearby jet collides, causing the filament toerupt faster. These results provide evidence that RNF plays an important rolein the formation and eruption of the sigmoidal filament. The phenomena alsosuggests that the kink instability is the trigger mechanism for the filamenteruption.

The Formation and Eruption of A Sigmoidal Filament Driven by Rotating Network Magnetic Fields