The detailed observational analysis of a homologous Extreme-ultraviolet ( EUV ) wave event is presented to study the driving mechanism and the physical property of the EUV waves , combining high resolution data taken by the Solar Dynamics Observatory and the Solar TErrestrial RElations Observatory .
It is observed that four homologous EUV waves originated from the same active region AR11476 within about one hour , and the time separations between consecutive waves were of 8 – 20 minutes .
The waves showed narrow arc-shaped wavefronts and propagated in the same direction along a large-scale transequatorial loop system at a speed of 648 – 712 km s ^ { -1 } and a deceleration of 0.985 – 1.219 km s ^ { -2 } .
The EUV waves were accompanied by weak flares , coronal jets , and radio type iii bursts , in which the EUV waves were delayed with respect to the start times of the radio type iii bursts and coronal jets about 2 – 13 and 4 – 9 minutes , respectively .
Different to previous studies of homologous EUV waves , no coronal mass ejections were found in the present event .
Based on the observational results and the close temporal the spatial relationship between the EUV waves and the coronal jets , for the first time , we propose that the observed homologous EUV waves were large-amplitude nonlinear fast-mode magnetosonic waves or shocks driven by the associated recurrent coronal jets , resemble the generation mechanism of a piston shock in a tube .
In addition , it is found that the recurrent jets were tightly associated with the alternating flux cancellation and emergence in the eruption source region and radio type iii bursts .