# Kinematics and Energetics of the EUV Waves on 11 April 2013

## TL;DR

This study analyzes EUV waves associated with a solar flare, revealing fast and slow components, stationary wave fronts, wave conversion phenomena, and energy estimates, enhancing understanding of solar coronal dynamics.

## Contribution

It provides detailed observations of EUV wave components, stationary fronts, and wave conversion processes during a solar flare event, which were not previously documented in this detail.

## Key findings

- Fast EUV wave speeds range from 600 to 640 km/s.
- Stationary wave fronts form at magnetic quasi-separatrix layers.
- EUV wave energy is estimated at approximately 10^20 Joules.

## Abstract

In this study, we present the observations of extreme-ultraviolet (EUV) waves associated with an M6.5 flare on 2013 April 11. The event was observed by Solar Dynamics Observatory (SDO) in different EUV channels. The flare was also associated with a halo CME and type II radio bursts. We observed both fast and slow components of the EUV wave. The speed of the fast component, which is identified as a fast-mode MHD wave, varies in the range from 600 to 640 km s^-1 , whereas the speed of the slow-component is ~140 km s^-1 . We observed an unusual phenomenon that, as the fast-component EUV wave passes through two successive magnetic quasi-separatrix layers (QSLs), two stationary wave fronts are formed locally. We propose that part of the outward-propagating fast-mode EUV wave is converted into slow-mode magnetohydrodynamic waves, which are trapped in local magnetic field structures, forming successive stationary fronts. Along the other direction, the fast-component EUV wave also creates oscillations in a coronal loop lying ~225 Mm away from the flare site. We have computed the energy of the EUV wave to be of the order of 10^20 J.