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tokens: rotated about 1.1 turns. Accompanied by the rotation, some fine dark threads moved as a whole from the southeast to the northwest to the coronal loops (Figures 2 (a)–(f)). At last, most of the threads interacted with the overlying field (see also Figure 4 (f)). In this process, a circular ribbon developed at the site of filament eruption as indicated in Figures 2 (b) and (e). By 09:04 UT, an interaction between the shifting filament and the coronal loops occurred and a brightening of the filament appeared at the reconnection sites (indicated by the white arrow in Figure 2 (f)). The brightened plasma around the reconnection region may be heated to higher temperature. Meanwhile, the reconnection resulted in the formation of some newly closed hot loops connecting “P” to “N1” (indicated in Figure 2 (i)). From AIA 304 Å observations at 09:06 UT, the filament was split and disintegrated completely. It is clear that the draining process is not freely falling but shaped by the magnetic field, and the bulk of filament mass flowed away along the nearby magnetic field, taking the shape of a jet (Figures 2 (g) and (h)). Figure 2. AIA 94, 304 Å, and H α images showing the eruptive process of the filament and subsequent interaction between the filament and coronal loops. (a–c) H α images showing the filament eruption. The solid arrow in panel (c) denotes the shift movement of the filament during filament rising. (d–g) 304 Å images showing the eruptive filament colliding with coronal loops. The blue and white contours have the same meaning as in Figure 1 . The coronal loops originating from “N1” are superposed with white lines, such as in panel (d) of Figure 1 . (h, i) Close-up views of the interacting region at AIA 304 and 94 Å, for which the FOV is indicated by the dashed line box in panel (f). Panel (i) is a 94 Å image showing newly formed hot loops. The white lines with an arrow (slice1 and slice2) mark the slit position of time slices as shown in Figure 3 (c) and (f), respectively. The white box of panel (g) indicates the FOV for Figure 4 . The animated version of this figure compares the AIA 94, 211, and 304 Å images from 08:40 to 09:10 UT compressed to a 5 s movie. (An animation of this figure is available.) Figure 3. (a–c) H α images showing an unwinding motion of filament (counterclockwise from above). A curved arrow indicates the direction. (d) Time slice taken from H α images at the position marked by slice3 in panel (b). A strand rotating around the filament is highlighted by the white dotted line. Figure 4. (a, b) Normalized light curves of AIA 94, 304, 335, and 1600 Å, and the positive magnetic flux. Fermi HXR 10–14 keV and 14–25 keV fluxes are also plotted. The AIA curves and magnetic flux are calculated from the eruptive region outlined by the white box in panel (f) of Figure 2 . (c) Time-slice plot for the shift motion of the eruptive filament along slice1 in Figure 2 (c), with the white lines marking the filament threads. The two