Light walls , as ensembles of oscillating bright structures rooted in sunspot light bridges , have not been well studied , although they are important for understanding sunspot properties .
Using the Interface Region Imaging Spectrograph and Solar Dynamics Observatory observations , here we study the evolution of two oscillating light walls each within its own active region ( AR ) .
The emission of each light wall decays greatly after the appearance of adjacent brightenings .
For the first light wall , rooted within AR 12565 , the average height , amplitude , and oscillation period significantly decrease from 3.5 Mm , 1.7 Mm , and 8.5 min to 1.6 Mm , 0.4 Mm , and 3.0 min , respectively .
For the second light wall , rooted within AR 12597 , the mean height , amplitude , and oscillation period of the light wall decrease from 2.1 Mm , 0.5 Mm , and 3.0 min to 1.5 Mm , 0.2 Mm , and 2.1 min , respectively .
Particularly , a part of the second light wall becomes even invisible after the influence of nearby brightening .
These results reveal that the light walls are suppressed by nearby brightenings .
Considering the complex magnetic topology in light bridges , we conjecture that the fading of light walls may be caused by a drop in the magnetic pressure , where flux is cancelled by magnetic reconnection at the site of the nearby brightening .
Another hypothesis is that the wall fading is due to the suppression of driver source ( p -mode oscillation ) , resulting from the nearby avalanche of downward particles along reconnected brightening loops .