For the first time , we report a large-scale wave that was observed simultaneously in the photosphere , chromosphere , transition region and low corona layers of the solar atmosphere .
Using the high temporal and high spatial resolution observations taken by the Solar Magnetic Activity Research Telescope at Hida Observatory and the Atmospheric Imaging Assembly ( AIA ) onboard Solar Dynamic Observatory , we find that the wave evolved synchronously at different heights of the solar atmosphere , and it propagated at a speed of 605 km s ^ { -1 } and showed a significant deceleration ( -424 m s ^ { -2 } ) in the extreme-ultraviolet ( EUV ) observations .
During the initial stage , the wave speed in the EUV observations was 1000 km s ^ { -1 } , similar to those measured from the AIA 1700 Å ( 967 km s ^ { -1 } ) and 1600 Å ( 893 km s ^ { -1 } ) observations .
The wave was reflected by a remote region with open fields , and a slower wave-like feature at a speed of 220 km s ^ { -1 } was also identified following the primary fast wave .
In addition , a type-II radio burst was observed to be associated with the wave .
We conclude that this wave should be a fast magnetosonic shock wave , which was firstly driven by the associated coronal mass ejection and then propagated freely in the corona .
As the shock wave propagated , its legs swept the solar surface and thereby resulted in the wave signatures observed in the lower layers of the solar atmosphere .
The slower wave-like structure following the primary wave was probably caused by the reconfiguration of the low coronal magnetic fields , as predicted in the field-line stretching model .