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Utilizing observations from the New Vacuum Solar Telescope (NVST), SolarDynamics Observatory (SDO), and Solar Terrestrial Relations Observatory-Ahead(STEREO-A), we investigate the event from two distinct observationalperspectives: on the solar disk using NVST and SDO, and on the solar limb usingSTEREO-A. We employ both a non-linear force-free field model and a potentialfield model to reconstruct the coronal magnetic field, aiming to understand itsmagnetic properties. Two precursor jet-like activities were observed before theeruption, displaying an untwisted rotation. The second activity released anestimated twist of over two turns. During these two jet-like activities,Y-shaped brightenings, newly emerging magnetic flux accompanied by magneticcancellation, and the formation of newly moving fibrils were identified.Combining these observational features, it can be inferred that these twoprecursor jet-like activities released the magnetic field constraining thefilament and were triggered by newly emerging magnetic flux. Before thefilament eruption, it was observed that some moving flows had been ejected fromthe site as the onset of two jet-like activities, indicating the same physicalprocess as two jet-like activities. Extrapolations revealed that the filamentlaid under the height of the decay index of 1.0 and had strong magnetic field(540 Gauss) and a high twisted number (2.4 turns) before the eruption. Anapparent rotational motion was observed during the filament eruption. We deducethat the solar filament, exhibiting an inverted U-shape, is a significantlytwisted flux rope. The eruption of the filament was initiated by the release ofconstraining magnetic fields through continuous magnetic reconnection. Thisreconnection process was triggered by the emergence of newly magnetic flux.

Onset mechanism of an inverted U-shaped solar filament eruption revealed by NVST, SDO, and STEREO-A observations