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ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS EJECTION CURRENT SHEETS
Murphy, NA1; Miralles, MP1; Pope, CL1,2; Raymond, JC1; Winter, HD1; Reeves, KK1; Seaton, DB3; van Ballegooijen, AA1; Lin J(林隽)1,4; Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
发表期刊ASTROPHYSICAL JOURNAL
2012-05-20
卷号751期号:1
DOI10.1088/0004-637X/751/1/56
产权排序第4完成单位
收录类别SCI
关键词Magnetic Reconnection Methods: Numerical Sun: Coronal Mass Ejections (Cmes) Sun: Flares
摘要We present two-dimensional resistive magnetohydrodynamic simulations of line-tied asymmetric magnetic reconnection in the context of solar flare and coronal mass ejection current sheets. The reconnection process is made asymmetric along the inflow direction by allowing the initial upstream magnetic field strengths and densities to differ, and along the outflow direction by placing the initial perturbation near a conducting wall boundary that represents the photosphere. When the upstream magnetic fields are asymmetric, the post-flare loop structure is distorted into a characteristic skewed candle flame shape. The simulations can thus be used to provide constraints on the reconnection asymmetry in post-flare loops. More hard X-ray emission is expected to occur at the footpoint on the weak magnetic field side because energetic particles are more likely to escape the magnetic mirror there than at the strong magnetic field footpoint. The footpoint on the weak magnetic field side is predicted to move more quickly because of the requirement in two dimensions that equal amounts of flux must be reconnected from each upstream region. The X-line drifts away from the conducting wall in all simulations with asymmetric outflow and into the strong magnetic field region during most of the simulations with asymmetric inflow. There is net plasma flow across the X-line for both the inflow and outflow directions. The reconnection exhaust directed away from the obstructing wall is significantly faster than the exhaust directed toward it. The asymmetric inflow condition allows net vorticity in the rising outflow plasmoid which would appear as rolling motions about the flux rope axis.
项目资助者NASA [NNX09AB17G, NNX11AB61G, NNM07AB07C, NNX09AH22G] ; NSF-REU at the Center for Astrophysics [ATM-0851866] ; NSF-SHINE [ATM0752257] ; Program 973 [2011CB811403] ; NSFC [10873030] ; CAS [KJCX2-EW-T07, 2010Y2JB16] ; Belgian Federal Science Policy Office through ESA-PRODEX [4000103240] ; NASA through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-637X
URL查看原文
WOS记录号WOS:000303814600056
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]HARD X-RAY ; ORDER FINITE-ELEMENTS ; FIELD LINE SHRINKAGE ; INITIAL PITCH-ANGLE ; CME CURRENT SHEETS ; FOOTPOINT EMISSIONS ; SUPRA-ARCADE ; MOTIONS ; LOOPS ; PROMINENCES
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6203
专题太阳物理研究组
通讯作者Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
作者单位1.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
2.Elmhurst College, Elmhurst, IL, USA
3.SIDC-Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Brussels, Belgium
4.Yunnan Astronomical Observatory, Chinese Academy of Sciences, P.O. Box 110, Kunming, Yunnan 650011, China
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Murphy, NA,Miralles, MP,Pope, CL,et al. ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS EJECTION CURRENT SHEETS[J]. ASTROPHYSICAL JOURNAL,2012,751(1).
APA Murphy, NA.,Miralles, MP.,Pope, CL.,Raymond, JC.,Winter, HD.,...&Murphy, NA .(2012).ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS EJECTION CURRENT SHEETS.ASTROPHYSICAL JOURNAL,751(1).
MLA Murphy, NA,et al."ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS EJECTION CURRENT SHEETS".ASTROPHYSICAL JOURNAL 751.1(2012).
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