Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. III. Shock-Associated CME/EUV Wave in an Event with a Two-Component EUV Transient

TL;DR

This study analyzes a 2010 solar event where a coronal shock wave and EUV waves were observed, revealing two EUV components linked to a CME and a shock wave, with detailed kinematic analysis supporting shock wave formation by filament eruption.

Contribution

It identifies and characterizes two EUV components associated with a CME and shock wave, providing detailed kinematic analysis and linking EUV features to shock wave dynamics.

Findings

The shock wave matched expectations for a freely expanding coronal shock.

The transient's speed was consistent with EUV wave characteristics.

The CME expansion was well described by a power-law fit.

Abstract

On 17 January 2010, STEREO-B observed in extreme ultraviolet (EUV) and white light a large-scale dome-shaped expanding coronal transient with perfectly connected off-limb and on-disk signatures. Veronig et al. (2010, ApJL 716, 57) concluded that the dome was formed by a weak shock wave. We have revealed two EUV components, one of which corresponded to this transient. All of its properties found from EUV, white light, and a metric type II burst match expectations for a freely expanding coronal shock wave including correspondence to the fast-mode speed distribution, while the transient sweeping over the solar surface had a speed typical of EUV waves. The shock wave was presumably excited by an abrupt filament eruption. Both a weak shock approximation and a power-law fit match kinematics of the transient near the Sun. Moreover, the power-law fit matches expansion of the CME leading edge up to 24 solar radii. The second, quasi-stationary EUV component near the dimming was presumably associated with a stretched CME structure; no indications of opening magnetic fields have been detected far from the eruption region.