  Extreme-ultraviolet (EUV) waves are one of the large-scale phenomena on the
Sun. They are defined as large propagating fronts in the low corona with speeds
ranging from a few tens km/s to a multiple of 1000 km/s. They are often
associated with solar filament eruptions, flares, or coronal mass ejections
(CMEs). EUV waves show different features, such as, wave and nonwave
components, stationary fronts, reflection, refraction, and mode conversion.
Apart from these, they can hit the nearby coronal loops and
filaments/prominences during their propagation and trigger them to oscillate.
These oscillating loops and filaments/prominences enable us to diagnose coronal
parameters such as the coronal magnetic field strength. In this article, we
present the different observed features of the EUV waves along with existing
models.
