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 × 10 4 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.
Description
Observations and Interpretation of a Low Coronal Shock Wave Observed in the EUV by the SDO/AIA
%0 Journal Article
%1 AiaShock
%A Ma, Suli
%A Raymond, John C.
%A Golub, Leon
%A Lin, Jun
%A Chen, Huadong
%A Grigis, Paolo
%A Testa, Paola
%A Long, David
%D 2011
%J The Astrophysical Journal
%K cme corona plasma shock
%N 2
%P 160
%T Observations and Interpretation of a Low Coronal Shock Wave Observed in the EUV by the SDO/AIA
%U http://stacks.iop.org/0004-637X/738/i=2/a=160
%V 738
%X 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 × 10 4 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.
@article{AiaShock,
abstract = {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 × 10 4 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.},
added-at = {2012-02-15T12:43:19.000+0100},
author = {Ma, Suli and Raymond, John C. and Golub, Leon and Lin, Jun and Chen, Huadong and Grigis, Paolo and Testa, Paola and Long, David},
biburl = {https://www.bibsonomy.org/bibtex/22a1b4464cd01bf186049b254946f149e/ursg},
description = {Observations and Interpretation of a Low Coronal Shock Wave Observed in the EUV by the SDO/AIA},
interhash = {7f52dec5d4faf92ff5445ecdeac7be36},
intrahash = {2a1b4464cd01bf186049b254946f149e},
journal = {The Astrophysical Journal},
keywords = {cme corona plasma shock},
number = 2,
pages = 160,
timestamp = {2012-02-15T12:43:19.000+0100},
title = {Observations and Interpretation of a Low Coronal Shock Wave Observed in the EUV by the SDO/AIA},
url = {http://stacks.iop.org/0004-637X/738/i=2/a=160},
volume = 738,
year = 2011
}