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The excitation mechanism of coronal quasi-period fast-propagating (QFP) wavetrains remains unresolved. Using Atmospheric Imaging Assembly onboard the SolarDynamics Observatory observations, we study a narrow and a broad QFP wave trainexcited one after another during the successive eruptions of filaments hostedwithin a fan-spine magnetic system on 2013 October 20. The consecutiveoccurrence of these two types of QFP wave trains in the same event provides anexcellent opportunity to explore their excitation mechanisms and compare theirphysical parameters. Our observational results reveal that narrow and broad QFPwave trains exhibit distinct speeds, periods, energy fluxes, and relativeintensity amplitudes, although originating from the same active region andbeing associated with the same {\em GOES} C2.9 flare. Using wavelet analysis,we find that the narrow QFP wave train shares a similar period with the flareitself, suggesting its possible excitation through the pulsed energy release inthe magnetic reconnection process that generated the accompanying flare. On theother hand, the broad QFP wave train appears to be associated with the energypulses released by the successive expansion and unwinding of filament threads.Additionally, it is plausible that the broad QFP wave train was also excited bythe sequential stretching of closed magnetic field lines driven by the eruptingfilament. These findings shed light on the different excitation mechanisms andorigins of the QFP wave trains.

Consecutive Narrow and Broad Quasi-periodic Fast-propagating Wave Trains Associated with a Flare