Authors: Wei Liu (Lockheed Martin Solar and Astrophysics Laboratory and Bay Area Environmental Research Institute), Meng Jin (Lockheed Martin Solar and Astrophysics Laboratory), Tongjiang Wang (Catholic University of America and NASA Goddard Space Flight Center), Leon Ofman (Catholic University of America and NASA Goddard Space Flight Center), Xudong Sun (University of Hawaii)

The dynamic, magnetized solar corona hosts a variety of plasma or magnetohydrodynamic (MHD) waves that are believed to play important roles in many fundamental, yet enigmatic processes, such as energy transport and corona heating. They also carry critical information that can be used to decipher the elusive physical parameters of the corona, such as the magnetic-field strength, by a technique called coronal seismology. In particular, large-scale extreme ultraviolet (EUV) waves associated with coronal mass ejections (CMEs) and solar flares, partly because of their large amplitudes, can provide novel diagnostics of the solar corona on global scales, an area yet to be fully exploited, compared to conventional local coronal seismology using loop oscillations. We will present recent advances on this subject, focusing on detailed analysis of various behaviors, such as reflection and refraction of well-observed EUV wave events, including the SOL2017-09-10 X8.2 flare. We will also present data-constrained simulations of these events, using state-of-the-art 3D MHD codes. By comparing the observations and simulations, we benchmark diagnostics of the magnetic field strengths and thermal properties of the solar corona. In addition, we will present statistical analysis of a large sample of the so-called quasi-periodic fast-mode propagating (QFP) wave trains, with a focus on their preferential association with eruptive flares (i.e., those associated with CMEs), as opposed to confined flares. We discuss the broader implications of these results for global coronal seismology and beyond.