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Deformation and deceleration of coronal wave
Xue ZK(薛志科)1,3; Qu ZQ(屈中权)1; Yan XL(闫晓理)1,2; Zhao, L4; Ma L(马琳)1,3; Xue, ZK (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
发表期刊ASTRONOMY & ASTROPHYSICS
2013-08
卷号556页码:152-158
DOI10.1051/0004-6361/201220731
产权排序第1完成单位
收录类别SCI ; EI
关键词Sun: Activity Sun: Corona Sun: Magnetic Topology Waves
摘要Aims. We studied the kinematics and morphology of two coronal waves to better understand the nature and origin of coronal waves. Methods. Using multi-wavelength observations of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) and the Extreme Ultraviolet Imager (EUVI) on board the twin spacecraft Solar-TErrestrial RElations Observatory (STEREO), we present morphological and dynamic characteristics of consecutive coronal waves on 2011 March 24. We also show the coronal magnetic field based on the potential field source surface model. Results. This event contains several interesting aspects. The first coronal wave initially appeared after a surge-like eruption. Its front was changed and deformed significantly from a convex shape to a line-shaped appearance, and then to a concave configuration during its propagation to the northwest. The initial speeds ranged from 947 km s(-1) to 560 km s(-1). The first wave decelerated significantly after it passed through a filament channel. After the deceleration, the final propagation speeds of the wave were from 430 km s(-1) to 312 km s(-1). The second wave was found to appear after the first wave in the northwest side of the filament channel. Its wave front was more diffused and the speed was around 250 km s(-1), much slower than that of the first wave. Conclusions. The deformation of the first coronal wave was caused by the different speeds along different paths. The sudden deceleration implies that the refraction of the first wave took place at the boundary of the filament channel. The event provides evidence that the first coronal wave may be a coronal MHD shock wave, and the second wave may be the apparent propagation of the brightenings caused by successive stretching of the magnetic field lines.
项目资助者National Science Foundation of China (NSFC) [10903027, 11078005, 10943002, 11103075] ; Key Laboratory of Solar Activity of CAS [KLSA201303] ; China's 973 project [G2011CB811400]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6361
URL查看原文
归档日期2013-09-24
WOS记录号WOS:000323893500152
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]EXTREME-ULTRAVIOLET WAVE ; GLOBAL EUV WAVE ; EIT WAVES ; MASS EJECTION ; MORETON WAVES ; SOLAR CORONA ; PROPAGATING DISTURBANCE ; QUADRATURE OBSERVATIONS ; SOHO/EIT OBSERVATIONS ; NUMERICAL-SIMULATION
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6226
专题太阳物理研究组
通讯作者Xue, ZK (reprint author), Chinese Acad Sci, Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
作者单位1.National Astronomical Observatories/Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming, 650011 Yunnan, PR China
2.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China
3.University of Chinese Academy of Sciences, 100049 Beijing, PR China c
4.Yunnan Normal University, 650092 Kunming Yunnan, PR China
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Xue ZK,Qu ZQ,Yan XL,et al. Deformation and deceleration of coronal wave[J]. ASTRONOMY & ASTROPHYSICS,2013,556:152-158.
APA Xue ZK,Qu ZQ,Yan XL,Zhao, L,Ma L,&Xue, ZK .(2013).Deformation and deceleration of coronal wave.ASTRONOMY & ASTROPHYSICS,556,152-158.
MLA Xue ZK,et al."Deformation and deceleration of coronal wave".ASTRONOMY & ASTROPHYSICS 556(2013):152-158.
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