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FORMATION OF A DOUBLE-DECKER MAGNETIC FLUX ROPE IN THE SIGMOIDAL SOLAR ACTIVE REGION 11520
Cheng, X1,2,3; Ding, MD1,3; Zhang, J1,4; Sun, XD5; Guo, Y1,3; Wang, YM6; Berhard Kliem7,8; Deng, YY2
Source PublicationASTROPHYSICAL JOURNAL
2014-07-10
Volume789Issue:2
DOI10.1088/0004-637X/789/2/93
Contribution Rank第8完成单位
Indexed BySCI
KeywordSun: coronaSun: corona Sun: coronal mass ejections (CMEs) Sun: filaments, prominences Sun: magnetic fields
Abstract

In this paper, we address the formation of a magnetic flux rope (MFR) that erupted on 2012 July 12 and caused a strong geomagnetic storm event on July 15. Through analyzing the long-term evolution of the associated active region observed by the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, it is found that the twisted field of an MFR, indicated by a continuous S-shaped sigmoid, is built up from two groups of sheared arcades near the main polarity inversion line a half day before the eruption. The temperature within the twisted field and sheared arcades is higher than that of the ambient volume, suggesting that magnetic reconnection most likely works there. The driver behind the reconnection is attributed to shearing and converging motions at magnetic footpoints with velocities in the range of 0.1-0.6 km s(-1). The rotation of the preceding sunspot also contributes to the MFR buildup. Extrapolated three-dimensional non-linear force-free field structures further reveal the locations of the reconnection to be in a bald-patch region and in a hyperbolic flux tube. About 2 hr before the eruption, indications of a second MFR in the form of an S-shaped hot channel are seen. It lies above the original MFR that continuously exists and includes a filament. The whole structure thus makes up a stable double-decker MFR system for hours prior to the eruption. Eventually, after entering the domain of instability, the high-lying MFR impulsively erupts to generate a fast coronal mass ejection and X-class flare; while the low-lying MFR remains behind and continuously maintains the sigmoidicity of the active region.

Funding ProjectNSFC[10933003] ; NSFC[11303016] ; NSFC[11373023] ; NSFC[11203014] ; NKBRSF[2011CB811402] ; NKBRSF[2014CB744203] ; Key Laboratory of Solar Activity of National Astronomical Observatories of the Chinese Academy of Sciences[KLSA201311] ; NSF[ATM-0748003] ; NSF[AGS-1156120] ; NSF[AGS-1249270] ; DFG ; ChineseAcademy of Sciences[2012T1J0017]
Funding OrganizationNSFC[10933003, 11303016, 11373023, 11203014] ; NKBRSF[2011CB811402, 2014CB744203] ; Key Laboratory of Solar Activity of National Astronomical Observatories of the Chinese Academy of Sciences[KLSA201311] ; NSF[ATM-0748003, AGS-1156120, AGS-1249270] ; DFG ; ChineseAcademy of Sciences[2012T1J0017]
Language英语
Subject Area天文学 ; 太阳与太阳系 ; 太阳物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS IDWOS:000338674900002
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCORONAL MASS EJECTIONS ; EMISSION MEASURE ANALYSIS ; X-RAY TELESCOPE ; VECTOR MAGNETOGRAPH ; INDUCTION EQUATION ; TUBE EMERGENCE ; ERUPTION ; EVOLUTION ; PROMINENCE ; FIELD
Citation statistics
Cited Times:61[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6246
Collection太阳物理研究组
Corresponding AuthorCheng, X
Affiliation1.School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China
2.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
3.Key Laboratory for Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China
4.School of Physics, Astronomy and Computational Sciences, George Mason University, Fairfax, VA 22030, USA
5.W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
6.School of Earth and Space Sciences, University of Science and Technology of China, Hefei 230026, China
7.Institute of Physics and Astronomy, University of Potsdam, D-14476 Potsdam, Germany
8.Yunnan Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan 650011, China
Recommended Citation
GB/T 7714
Cheng, X,Ding, MD,Zhang, J,et al. FORMATION OF A DOUBLE-DECKER MAGNETIC FLUX ROPE IN THE SIGMOIDAL SOLAR ACTIVE REGION 11520[J]. ASTROPHYSICAL JOURNAL,2014,789(2).
APA Cheng, X.,Ding, MD.,Zhang, J.,Sun, XD.,Guo, Y.,...&Deng, YY.(2014).FORMATION OF A DOUBLE-DECKER MAGNETIC FLUX ROPE IN THE SIGMOIDAL SOLAR ACTIVE REGION 11520.ASTROPHYSICAL JOURNAL,789(2).
MLA Cheng, X,et al."FORMATION OF A DOUBLE-DECKER MAGNETIC FLUX ROPE IN THE SIGMOIDAL SOLAR ACTIVE REGION 11520".ASTROPHYSICAL JOURNAL 789.2(2014).
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