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Quasi-periodic, fast-mode, propagating wave trains (QFPs) are a newobservational phenomenon recently discovered in the solar corona by the SolarDynamics Observatory with extreme ultraviolet (EUV) imaging observations. Theyoriginate from flares and propagate at speeds up to ~2000 km/s withinfunnel-shaped waveguides in the wakes of coronal mass ejections (CMEs). QFPscan carry sufficient energy fluxes required for coronal heating during theiroccurrences. They can provide new diagnostics for the solar corona and theirassociated flares. We present recent observations of QFPs focusing on theirspatio-temporal properties, temperature dependence, and statistical correlationwith flares and CMEs. Of particular interest is the 2010-Aug-01 C3.2 flare withcorrelated QFPs and drifting zebra and fiber radio bursts, which might bedifferent manifestations of the same fast-mode wave trains. We also discuss thepotential roles of QFPs in accelerating and/or modulating the solar wind.

Quasi-periodic Fast-mode Magnetosonic Wave Trains Within Coronal Waveguides Associated with Flares and CMEs