With the high tempo-spatial Interface Region Imaging Spectrograph 1330 Å images , we find that many bright structures are rooted in the light bridge of NOAA 12192 , forming a light wall .
The light wall is brighter than the surrounding areas , and the wall top is much brighter than the wall body .
The New Vacuum Solar Telescope H \alpha and the Solar Dynamics Observatory 171 Å and 131 Å images are also used to study the light wall properties .
In 1330 Å , 171 Å , and 131 Å , the top of the wall has a higher emission , while in the H \alpha line , the wall top emission is very low .
The wall body corresponds to bright areas in 1330 Å and dark areas in the other lines .
The top of the light wall moves upward and downward successively , performing oscillations in height .
The deprojected mean height , amplitude , oscillation velocity , and the dominant period are determined to be 3.6 Mm , 0.9 Mm , 15.4 km s ^ { -1 } , and 3.9 min , respectively .
We interpret the oscillations of the light wall as the leakage of p -modes from below the photosphere .
The constant brightness enhancement of the wall top implies the existence of some kind of atmospheric heating , e.g. , via the persistent small-scale reconnection or the magneto-acoustic waves .
In another series of 1330 Å images , we find that the wall top in the upward motion phase is significantly brighter than in the downward phase .
This kind of oscillations may be powered by the energy released due to intermittent impulsive magnetic reconnection .