We present two events to study the driving mechanism of extreme-ultraviolet ( EUV ) waves that are not associated with coronal mass ejections ( CMEs ) , by using high resolution observations taken by the Atmospheric Imaging Assembly ( AIA ) on board Solar Dynamics Observatory .
Observational results indicate that the observed EUV waves were accompanied by flares and coronal jets , but without CMEs that were regarded as the driver of most EUV waves in previous studies .
In the first case , it is observed that a coronal jet ejected along a transequatorial loop system at a plane-of-the-sky ( POS ) speed of 335 \pm 22 km s ^ { -1 } , in the meantime , an arc-shaped EUV wave appeared on the eastern side of the loop system .
In addition , the EUV wave further interacted with another interconnecting loop system and launched a fast propagating ( QFP ) magnetosonic wave along the loop system , which had a period of 200 s and a speed of 388 \pm 65 km s ^ { -1 } , respectively .
In the second case , we also observed a coronal jet ejected at a POS speed of 282 \pm 44 km s ^ { -1 } along a transequatorial loop system and the generation of bright EUV wave on the eastern side of the loop system .
Based on the observational results , we propose that the observed EUV waves on the eastern side of the transequatorial loop systems are fast-mode magnetosonic waves , and they were driven by the sudden lateral expansion of the transequatorial loop systems due to the direct impingement of the associated coronal jets , while the QFP wave in the fist case formed due to the dispersive evolution of the disturbance caused by the interaction between the EUV wave and the interconnecting coronal loops .
It is noted that EUV waves driven by sudden loop expansions have shorter lifetimes than those driven by CMEs .