Mode-Conversion of a Solar Extreme-Ultraviolet Wave over a Coronal Cavity

TL;DR

This study observes an EUV wave on the Sun that undergoes mode conversion when interacting with a coronal cavity, revealing complex wave-CME interactions and providing insights into solar wave dynamics.

Contribution

It presents evidence of mode conversion of an EUV wave over a coronal cavity, linking wave behavior to magnetic field interactions and advancing understanding of solar wave phenomena.

Findings

The wave's trailing edge stops at the cavity, while the leading edge extends and intensifies.

The wave experiences significant deceleration and intensification over the cavity.

Mode conversion from fast-mode to slow-mode wave explains the observed wave behavior.

Abstract

We report on observations of an extreme-ultraviolet (EUV) wave event in the Sun on 2011 January 13 by \emph{Solar Terrestrial Relations Observatory} (\emph{STEREO}) and \emph{Solar Dynamics Observatory} (\emph{SDO}) in quadrature. Both the trailing edge and the leading edge of the EUV wave front in the north direction are reliably traced, revealing generally compatible propagation velocities in both perspectives and a velocity ratio of about 1/3. When the wave front encounters a coronal cavity near the northern polar coronal hole, the trailing edge of the front stops while its leading edge just shows a small gap and extends over the cavity, meanwhile getting significantly decelerated but intensified. We propose that the trailing edge and the leading edge of the northward propagating wave front correspond to a non-wave coronal mass ejection (CME) component and a fast-mode magnetohydrodynamic (MHD) wave component, respectively. The interaction of the fast-mode wave and the coronal cavity may involve a mode conversion process, through which part of the fast-mode wave is converted to a slow-mode wave that is trapped along the magnetic field lines. This scenario can reasonably account for the unusual behavior of the wave front over the coronal cavity.