摘要： Solar ?lament eruptions are often associated with solar ?ares and coronal mass ejections, which have the greatest impact on space weather. However, the ?ne structures and the trigger mechanisms of solar ?laments are still unclear. To address these issues, we studied a failed solar active-region ?lament eruption associated with a C-class ?are by using high-resolution Hα images from the New Vacuum Solar Telescope, supplemented by EUV observations from the Solar Dynamics Observatory. Before the ?lament eruption, a small bipolar magnetic ?eld emerged below the ?lament. Then magnetic reconnection between the ?lament and the emerging bipolar magnetic ?eld triggered the ?lament eruption. During the ?lament eruption, the untwisting motion of the ?lament can be clearly traced by the eruptive threads. Moreover, the footpoints of the eruptive threads are determined by tracing the descending ?lament material. Note that the twisted structure of the ?lament and the right part of the eruptive ?lament threads cannot be seen before the ?lament eruption. These eruptive threads in the right part of the ?lament are found to be rooting in the weak negative polarities near the main negative sunspot. Moreover, a new ?lament formed in the ?lament channel due to material injection from the eruptive ?lament. The above observations and the potential ?eld extrapolations are inclined to support the idea that the ?lament materials were transferred into the overlying magnetic loops and the nearby ?lament channel by magnetic reconnection. These observations improve our understanding of the complexity of ?lament eruptions.