  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 and a deceleration of 0.985 - 1.219 km/s2.
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.
