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Magnetic flux rope (MFR) is a coherent and helical magnetic field structurethat is recently found probably to appear as an elongated hot-channel prior toa solar eruption. In this paper, we investigate the relationship between thehot-channel and associated prominence through analyzing a limb event on 2011September 12. In the early rise phase, the hot-channel was cospatial with theprominence initially. It then quickly expanded, resulting in a separation ofthe top of the hot-channel from that of the prominence. Meanwhile, both of themexperienced an instantaneous morphology transformation from a $\Lambda$ shapeto a reversed-Y shape and the top of these two structures showed an exponentialincrease in height. These features are a good indication for the occurrence ofthe kink instability. Moreover, the onset of the kink instability is found tocoincide in time with the impulsive enhancement of the flare emissionunderneath the hot-channel, suggesting that the ideal kink instability likelyalso plays an important role in triggering the fast flare reconnection besidesinitiating the impulsive acceleration of the hot-channel and distorting itsmorphology. We conclude that the hot-channel is most likely the MFR system andthe prominence only corresponds to the cool materials that are collected in thebottom of the helical field lines of the MFR against the gravity.

On the Relationship Between a Hot-channel-like Solar Magnetic Flux Rope and its embedded Prominence