  The excitation mechanism of coronal quasi-period fast-propagating (QFP) wave
trains remains unresolved. Using Atmospheric Imaging Assembly onboard the Solar
Dynamics Observatory observations, we study a narrow and a broad QFP wave train
excited one after another during the successive eruptions of filaments hosted
within a fan-spine magnetic system on 2013 October 20. The consecutive
occurrence of these two types of QFP wave trains in the same event provides an
excellent opportunity to explore their excitation mechanisms and compare their
physical parameters. Our observational results reveal that narrow and broad QFP
wave trains exhibit distinct speeds, periods, energy fluxes, and relative
intensity amplitudes, although originating from the same active region and
being 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 flare
itself, suggesting its possible excitation through the pulsed energy release in
the magnetic reconnection process that generated the accompanying flare. On the
other hand, the broad QFP wave train appears to be associated with the energy
pulses released by the successive expansion and unwinding of filament threads.
Additionally, it is plausible that the broad QFP wave train was also excited by
the sequential stretching of closed magnetic field lines driven by the erupting
filament. These findings shed light on the different excitation mechanisms and
origins of the QFP wave trains.
