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NUMERICAL EXPERIMENTS ON FINE STRUCTURE WITHIN RECONNECTING CURRENT SHEETS IN SOLAR FLARES
Shen CC(沈呈彩)1,2; Lin J(林隽)1,3; Murphy, NA3; Shen, CC (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Yunnan, Peoples R China.
Source PublicationASTROPHYSICAL JOURNAL
2011-08-10
Volume737Issue:1
DOI10.1088/0004-637X/737/1/14
Contribution Rank第1完成单位
Indexed BySCI
KeywordInstabilities Magnetic Reconnection Magnetohydrodynamics (Mhd) Methods: Numerical Plasmas Sun: Flares
AbstractWe perform resistive magnetohydrodynamic simulations to study the internal structure of current sheets that form during solar eruptions. The simulations start with a vertical current sheet in mechanical and thermal equilibrium that separates two regions of the magnetic field with opposite polarity which are line-tied at the lower boundary representing the photosphere. Reconnection commences gradually due to an initially imposed perturbation, but becomes faster when plasmoids form and produce small-scale structures inside the current sheet. These structures include magnetic islands or plasma blobs flowing in both directions along the sheet, and X-points between pairs of adjacent islands. Among these X-points, a principal one exists at which the reconnection rate reaches maximum. A fluid stagnation point (S-point) in the sheet appeared where the reconnection outflow bifurcates. The S-point and the principal X-point (PX-point) are not co-located in space though they are very close to one another. Their relative positions alternate as reconnection progresses and determine the direction of motion of individual magnetic islands. Newly formed islands move upward if the S-point is located above the PX-point, and downward if the S-point is below the PX-point. Merging of magnetic islands was observed occasionally between islands moving in the same direction. Reconnected plasma flow was observed to move faster than blobs nearby.
Funding OrganizationProgram 973 [2011CB811403] ; NSFC [10873030] ; CAS [2009J2-34] ; NASA [NNX11AB61G] ; Smithsonian Institution
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0004-637X
URL查看原文
Archive Date2011-08-01
WOS IDWOS:000293332200014
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCORONAL MASS EJECTION ; FLUX-CORRECTED TRANSPORT ; MAGNETIC RECONNECTION ; 2-RIBBON FLARES ; ERUPTIONS ; LOOPS ; INFLOWS ; MOTIONS ; ARCADE ; MODEL
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Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6176
Collection太阳物理研究组
Corresponding AuthorShen, CC (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Yunnan, Peoples R China.
Affiliation1.Yunnan Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan 650011, China
2.Graduate School of the Chinese Academy of Sciences, Beijing 100039, China
3.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Shen CC,Lin J,Murphy, NA,et al. NUMERICAL EXPERIMENTS ON FINE STRUCTURE WITHIN RECONNECTING CURRENT SHEETS IN SOLAR FLARES[J]. ASTROPHYSICAL JOURNAL,2011,737(1).
APA Shen CC,Lin J,Murphy, NA,&Shen, CC .(2011).NUMERICAL EXPERIMENTS ON FINE STRUCTURE WITHIN RECONNECTING CURRENT SHEETS IN SOLAR FLARES.ASTROPHYSICAL JOURNAL,737(1).
MLA Shen CC,et al."NUMERICAL EXPERIMENTS ON FINE STRUCTURE WITHIN RECONNECTING CURRENT SHEETS IN SOLAR FLARES".ASTROPHYSICAL JOURNAL 737.1(2011).
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