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 |
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| Authors: | V V Grechnev A N Afanasyev A M Uralov I M Chertok M V Eselevich V G Eselevich G V Rudenko Y Kubo |
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| Institution: | (1) Institute of Solar-Terrestrial Physics SB RAS, Lermontov St. 126A, Irkutsk, 664033, Russia;(2) Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Troitsk, Moscow Region, 142190, Russia;(3) National Institute of Information and Communications Technology, Tokyo, Japan |
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| 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. (Astrophys. J. Lett.
716, L57, 2010) 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 with 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 the 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. |
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