OBSERVATIONS AND INTERPRETATION OF A LOW CORONAL SHOCK WAVE OBSERVED IN THE EUV BY THE SDO/AIA

By Suli Ma, J. C. Raymond, L. Golub, Jun Lin, Huadong Chen, P. Grigis, P. Testa, D. Long. 2011

142 citations recorded by the source corpus.

Taking advantage of both the high temporal and spatial resolutions of the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, we studied a limb coronal shock wave and its associated extreme ultraviolet (EUV) wave that occurred on 2010 June 13. Our main findings are: (1) the shock wave appeared clearly only in the channels centered at 193 Å and 211 Å as a dome-like enhancement propagating ahead of its associated semi-spherical coronal mass ejection (CME) bubble; (2) the density compression of the shock is 1.56 according to radio data and the temperature of the shock is around 2.8 MK; (3) the shock wave first appeared at 05:38 UT, 2 minutes after the associated flare has started and 1 minute after its associated CME bubble appeared; (4) the top of the dome-like shock wave set out from about 1.23 R☉ and the thickness of the shocked layer is ∼2 × 104 km; (5) the speed of the shock wave is consistent with a slight decrease from about 600 km s−1 to 550 km s−1; and (6) the lateral expansion of the shock wave suggests a constant speed around 400 km s−1, which varies at different heights and directions. Our findings support the view that the coronal shock wave is driven by the CME bubble, and the on-limb EUV wave is consistent with a fast wave or at least includes the fast wave component.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/23205909d06bcaf1b6d22dbe93f289eb4011896f

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Citations in the corpus

• Space weather: the solar perspective (2021, background): “However, the complex magnetic topology related to the active region prevents from making strong conclusions about the possible sites of particle acceleration (see also Kozarev et al. 2011; Ma et al. 2011; Gopalswamy et al. 2012).”
• Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “As shown in Figure 9d, among 138 events observed by AIA, 17% appear as 171 Å bright, 41% as dark, and the rest with no clear signal.”
• How Many CMEs Have Flux Ropes? Deciphering the Signatures of Shocks, Flux Ropes, and Prominences in Coronagraph Observations of CMEs (2012, background): “Recently, similar fronts have been detected in high cadence EUV images (Ma et al., 2011; Cheng et al., 2012).”