Extreme Ultraviolet ( EUV ) waves have been found for about 15 years .
However , significant controversy remains over their physical natures and origins .
In this paper , we report an EUV wave that was accompanied by an X1.9 flare and a partial halo coronal mass ejection .
Using high temporal and spatial resolution observations taken by the Solar Dynamics Observatory and the Solar-TErrestrial RElations Observatory , we are able to investigate the detailed kinematics of the EUV wave .
We find several arguments that support the fast-mode wave scenario : ( 1 ) The speed of the EUV wave ( 570 km s ^ { -1 } ) is higher than the sound speed of quiet-Sun corona .
( 2 ) Significant deceleration of the EUV wave ( -130 m s ^ { -2 } ) is found during its propagation .
( 3 ) The EUV wave resulted in the oscillations of a loop and a filament along its propagation path , and a reflected wave from the polar coronal hole is also detected .
( 4 ) Refraction or reflection effect is observed when the EUV wave was passing through two coronal bright points .
( 5 ) The dimming region behind the wavefront stopped to expand when the wavefront started to become diffuse .
( 6 ) The profiles of the wavefront exhibited a dispersive nature , and the magnetosonic Mach number of the EUV wave derived from the highest intensity jump is about 1.4 .
In addition , triangulation indicates that the EUV wave propagated within a height range of about 60–100 Mm above the photosphere .
We propose that the EUV wave observed should be a nonlinear fast-mode magnetosonic wave that propagated freely in the corona after it was driven by the CME expanding flanks during the initial period .