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

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.

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

“…However, the difference in the observed radial and lateral speeds could in principle result from different fast-mode speed profiles in the corresponding directions. Finally, Grechnev et al (2011) reached essentially the same conclusion using a 3D blast wave model which was in a very good agreement with the ground tracks of the wave dome both on-disk and off-limb. Other examples of wave domes can be seen in the events of 13 June 2010, 7 June 2011 and 4 August 2011.…”

“…The pulse broadening points also to a freely-propagating wave. Indeed, Grechnev et al (2011) found that a 3D model of a blast wave propagating in a medium with density stratification was broadly consistent with the ground track of 17 January 2010 (see also Veronig et al (2010)). Finally, MHD modeling of rotating sunspots by Selwa, Poedts, and DeVore (2012) showed that dome-like structures, similar to what is observed, could be generated.…”

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

“…The piston could thus be attributed to the front of the CME itself, or the full CME bubble or loops, as has been reported by several observational studies (Patsourakos and Vourlidas, 2012). Some observational reports reinforce this picture (Kienreich, Temmer, and Veronig, 2009;Patsourakos and Vourlidas, 2009;Veronig et al, 2010;Grechnev et al, 2011b). If this is the case, the faster lobe of sectors 29 -34 could be related with a piston provided by a CME structure, probably stretched, non-radially rising, i.e.…”

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

“…The enhanced pressure behind the wavefront compresses the chromospheric plasma, which is observed as the down-up swing in Hα filtergrams, and recently detected as EUV redshifts (Harra et al 2011;Veronig et al 2011) or seen in EUV images (Liu et al 2012b). As the Alfvén speed increases with height in the low corona, it is expected that the wavefront of a coronal fastmode MHD wave is forwardly inclined toward the solar surface, which is observed in some limb events (e.g., Hudson et al 2003;Liu et al 2012b) and reproduced by numerical simulations (e.g., Wu et al 2001;Grechnev et al 2011). In a recent observation, an Hα Moreton wavefront is observed to be the ground track of a dome-shaped coronal shock front (Asai et al 2012;Shen & Liu 2012).…”