  Using high temporal and high spatial resolution observations taken by the
Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we present
the detailed observational analysis of a high quality quasi-periodic fast-
propagating (QFP) magnetosonic wave that was associated with the eruption of a
magnetic flux rope and a GOES C5.0 flare. For the first time, we find that the
QFP wave lasted during the entire flare lifetime rather than only the rising
phase of the accompanying flare as reported in previous studies. In addition,
the propagation of the different parts of the wave train showed different
kinematics and morphologies. For the southern (northern) part, the speed,
duration, intensity variation are about 875 +/- 29 (1485 +/- 233) km/s, 45 (60)
minutes, and 4% (2%), and the pronounced periods of them are 106 +/- 12 and 160
+/- 18 (75 +/- 10 and 120 +/- 16) seconds, respectively. It is interesting that
the northern part of the wave train showed obvious refraction effect when they
pass through a region of strong magnetic field. Periodicity analysis result
indicates that all the periods of the QFP wave can be found in the period
spectrum of the accompanying flare, suggesting their common physical origin. We
propose that the quasi-periodic nonlinear magnetohydrodynamics process in the
magnetic reconnection that produces the accompanying flare should be important
for exciting of QFP wave, and the different magnetic distribution along
different paths can account for the different speeds and morphology evolution
of the wave fronts.
