In this paper , we report our multiwavelength observations of the vertical oscillation of a coronal cavity on 2011 March 16 .
The elliptical cavity with an underlying horn-like quiescent prominence was observed by the Atmospheric Imaging Assembly ( AIA ) on board the Solar Dynamics Observatory ( SDO ) .
The width and height of the cavity are 150 \arcsec and 240 \arcsec , and the centroid of cavity is 128 \arcsec above the solar surface .
At \sim 17:50 UT , a C3.8 two-ribbon flare took place in active region 11169 close to the solar western limb .
Meanwhile , a partial halo coronal mass ejection ( CME ) erupted and propagated at a linear speed of \sim 682 km s ^ { -1 } .
Associated with the eruption , a coronal extreme-ultraviolet ( EUV ) wave was generated and propagated in the northeast direction at a speed of \sim 120 km s ^ { -1 } .
Once the EUV wave arrived at the cavity from the top , it pushed the large-scale overlying magnetic field lines downward before bouncing back .
At the same time , the cavity started to oscillate coherently in the vertical direction and lasted for \sim 2 cycles before disappearing .
The amplitude , period , and damping time are 2.4 - 3.5 Mm , 29 - 37 minutes , and 26 - 78 minutes , respectively .
The vertical oscillation of the cavity is explained by a global standing MHD wave of fast kink mode .
To estimate the magnetic field strength of the cavity , we use two independent methods of prominence seismology .
It is found that the magnetic field strength is only a few Gauss and less than 10 G .