Observations of a Fast-mode Magnetosonic Wave Propagating along a Curving Coronal Loop on 2011 November 11

The detailed analysis of an interesting quasi-periodic fast-propagating (QFP) magnetosonic wave is presented using high-resolution observations taken by the Solar Dynamic Observatory. The QFP wave occurred over the west solar limb during the fast eruption phase of a nearby prominence. It propagated along a group of curving coronal loop and manifested two types of wave trains that showed different morphologies and propagation characteristics. The wavefronts of the first type wave trains are relatively broad, and they changed their propagation direction when they pass through the turning part of the guiding loop. On the contrary, the wavefronts of the other type wave trains are narrow, and their propagation did not affected by geometric changes of the guiding loop. Measurements indicate that the average speeds of the broad (narrow) wave trains is 305(343) {km} {{{s}}}^-1, and the period of the wave trains ranges from 54 to 458 s. We propose that the narrow wave trains may manifest the leakage of the wave trains from the guiding coronal loop, or were guided by another group of invisible coronal loop. In addition, the projection effect and weak magnetic field strength of the guiding coronal loop are proposed to explain the slow wave speed.