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Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology
文献类型：期刊论文
| 作者 | Jiang, Chaowei; Zou, Peng; Feng, Xueshang; Hu, Qiang; Liu, Rui; Vemareddy, P.; Duan, Aiying; Zuo, Pingbing; Wang, Yi; Wei, Fengsi |
| 刊名 | ASTROPHYSICAL JOURNAL
 |
| 出版日期 | 2018 |
| 卷号 | 869期号:1页码:13 |
| ISSN号 | 0004-637X |
| 关键词 | magnetic fields magnetohydrodynamics (MHD) methods: numerical Sun: corona Sun: flares |
| DOI | 10.3847/1538-4357/aaeacc |
| 英文摘要 | Three-dimensional magnetic topology is crucial to understanding the explosive release of magnetic energy in the corona during solar flares. Much attention has been given to the pre-flare magnetic topology to identify candidate sites of magnetic reconnection, yet it is unclear how the magnetic reconnection and its attendant topological changes shape the eruptive structure and how the topology evolves during the eruption. Here we employed a realistic, data-constrained magnetohydrodynamic simulation to study the evolving magnetic topology for an X9.3 eruptive flare that occurred on 2017 September 6. The simulation successfully reproduces the eruptive features and processes in unprecedented detail. The numerical results reveal that the pre-flare corona contains multiple twisted flux systems with different connections, and during the eruption these twisted fluxes form a coherent flux rope through tether-cutting-like magnetic reconnection below the rope. Topological analysis shows that the rising flux rope is wrapped by a quasi-separatrix layer, which intersects itself below the rope, forming a topological structure known as a hyperbolic flux tube, where a current sheet develops, triggering the reconnection. By mapping footpoints of the newly reconnected field lines, we are able to reproduce both the spatial location and, for the first time, the temporal separation of the observed flare ribbons, as well as the dynamic boundary of the flux rope's feet. Furthermore, the temporal profile of the total reconnection flux is comparable to the soft X-ray light curve. Such a sophisticated characterization of the evolving magnetic topology provides important insight into the eventual understanding and forecasting of solar eruptions. |
| 语种 | 英语 |
| 源URL | [http://ir.nssc.ac.cn/handle/122/6604]  |
| 专题 | 国家空间科学中心_空间科学部 |
| 推荐引用方式 GB/T 7714 | Jiang, Chaowei,Zou, Peng,Feng, Xueshang,et al. Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology[J]. ASTROPHYSICAL JOURNAL,2018,869(1):13. |
| APA | Jiang, Chaowei.,Zou, Peng.,Feng, Xueshang.,Hu, Qiang.,Liu, Rui.,...&Wei, Fengsi.(2018).Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology.ASTROPHYSICAL JOURNAL,869(1),13. |
| MLA | Jiang, Chaowei,et al."Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology".ASTROPHYSICAL JOURNAL 869.1(2018):13. |
入库方式： OAI收割
来源：国家空间科学中心
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