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.
@article{arxiv.2310.12844,
title = {Observational Characteristics of solar EUV waves},
author = {Ramesh Chandra and Pooja Devi and P. F. Chen and Brigitte Schmieder and Reetika Joshi and Bhuwan Joshi and Arun Kumar Awasthi},
journal= {arXiv preprint arXiv:2310.12844},
year = {2023}
}