ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS EJECTION CURRENT SHEETS
文献类型：期刊论文
| 作者 | Murphy, NA1; Miralles, MP1; Pope, CL1,2; Raymond, JC1; Winter, HD1; Reeves, KK1; Seaton, DB3; van Ballegooijen, AA1; Lin J(林隽)1,4
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| 刊名 | ASTROPHYSICAL JOURNAL
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| 出版日期 | 2012-05-20 |
| 卷号 | 751期号:1 |
| ISSN号 | 0004-637X |
| 关键词 | magnetic reconnection methods: numerical Sun: coronal mass ejections (CMEs) Sun: flares |
| 通讯作者 | Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. |
| 产权排序 | 第四完成单位 |
| 英文摘要 | 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. |
| 学科主题 | Astronomy & Astrophysics |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | 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 |
| 收录类别 | SCI |
| 原文出处 | http://iopscience.iop.org/article/10.1088/0004-637X/751/1/56/meta |
| 语种 | 英语 |
| WOS记录号 | WOS:000303814600056 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/6203]  |
| 专题 | 云南天文台_太阳物理研究组 |
| 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 |
| 推荐引用方式 GB/T 7714 | 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.,...&Lin J.(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). |
入库方式： OAI收割
来源：云南天文台
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