Winking ( oscillating ) filaments have been observed for many years .
However , observations of successive winking filaments in one event have not been reported yet .
In this paper , we present the observations of a chain of winking filaments and a subsequent jet that are observed right after the X2.1 flare in AR11283 .
The event also produced an Extreme-ultraviolet ( EUV ) wave that has two components : upward dome-like wave ( 850 km s ^ { -1 } ) and lateral surface wave ( 554 km s ^ { -1 } ) which was very weak ( or invisible ) in imaging observations .
By analyzing the temporal and spatial relationships between the oscillating filaments and the EUV waves , we propose that all the winking filaments and the jet were triggered by the weak ( or invisible ) lateral surface EUV wave .
The oscillation of the filaments last for two or three cycles , and their periods , Doppler velocity amplitudes , and damping times are 11 – 22 minutes , 6 – 14 km s ^ { -1 } , and 25 – 60 minutes , respectively .
We further estimate the radial component magnetic field and the maximum kinetic energy of the filaments , and they are 5 – 10 Gauss and \sim 10 ^ { 19 } { J } , respectively .
The estimated maximum kinetic energy is comparable to the minimum energy of ordinary EUV waves , suggesting that EUV waves can efficiently launch filament oscillations on their path .
Based on our analysis results , we conclude that the EUV wave is a good agent for triggering and connecting successive but separated solar activities in the solar atmosphere , and it is also important for producing solar sympathetic eruptions .