  Coronal disturbances associated with solar flares, such as H$\alpha$ Moreton
waves, X-ray waves, and extreme ultraviolet (EUV) coronal waves are discussed
herein in relation to magnetohydrodynamics fast-mode waves or shocks in the
corona. To understand the mechanism of coronal disturbances, full-disk solar
observations with high spatial and temporal resolution over multiple
wavelengths are of crucial importance. We observed a filament eruption, whose
shape is like a "dandelion", associated with the M1.6 flare that occurred on
2011 February 16 in the H$\alpha$ images taken by the Flare Monitoring
Telescope at Ica University, Peru. We derive the three-dimensional velocity
field of the erupting filament. We also identify winking filaments that are
located far from the flare site in the H$\alpha$ images, whereas no Moreton
wave is observed. By comparing the temporal evolution of the winking filaments
with those of the coronal wave seen in the extreme ultraviolet images data
taken by the Atmospheric Imaging Assembly on board the {\it Solar Dynamics
Observatory} and by the Extreme Ultraviolet Imager on board the {\it Solar
Terrestrial Relations Observatory-Ahead}, we confirm that the winking filaments
were activated by the EUV coronal wave.
