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On 2011 May 30, quasi-periodic fast propagating (QFP) magnetosonic wavesaccompanied by a C2.8 flare were directly imaged by the Atomospheric ImagingAssembly instrument on board the Solar Dynamics Observatory. The QFP wavessuccessively emanated from the flare kernel, they propagated along a cluster ofopen coronal loops with a phase speed of 834 km/s during the flare's risingphase, and the multiple arc-shaped wave trains can be fitted with a series ofconcentric circles. We generate the k-omega diagram of the Fourier power andfind a straight ridge that represents the dispersion relation of the waves.Along the ridge, we find a lot of prominent nodes which represent the availablefrequencies of the QFP waves. On the other hand, the frequencies of the flareare also obtained by analyzing the flare light curves using the wavelettechnique. The results indicate that almost all the main frequencies of theflare are consistent with those of the QFP waves. This suggests that the flareand the QFP waves were possibly excited by a common physical origin. On theother hand, a few low frequencies revealed by the k-omega diagram can not befound in the accompanying flare. We propose that these low frequencies werepossibly due to the leakage of the pressure-driven p-mode oscillations from thephotosphere into the low corona, which should be a noticeable mechanism fordriving the QFP waves observed in the corona.

Observational Study Of the Quasi-Periodic Fast Propagating Magnetosonic Waves and the Associated Flare on 2011 May 30