Magnetohydrodynamic Turbulence Formation in Solar Flares: 3D Simulation and Synthetic Observations
文献类型：期刊论文
| 作者 | Ruan,W.2; Yan,L.1; Keppens,R.2 |
| 刊名 | The Astrophysical Journal
 |
| 出版日期 | 2023-04-01 |
| 卷号 | 947期号:2 |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/ac9b4e |
| 英文摘要 | Abstract Turbulent plasma motion is common in the universe and invoked in solar flares to drive effective acceleration leading to high-energy electrons. Unresolved mass motions are frequently detected in flares from extreme ultraviolet (EUV) observations, which are often regarded as turbulence. However, how this plasma turbulence forms during the flare is still largely a mystery. Here we successfully reproduce observed turbulence in our 3D magnetohydrodynamic simulation where the magnetic reconnection process is included. The turbulence forms as a result of an intricate nonlinear interaction between the reconnection outflows and the magnetic arcades below the reconnection site, in which the shear-flow-driven Kelvin–Helmholtz instability (KHI) plays a key role in generating turbulent vortices. The turbulence is produced above high-density flare loops and then propagates to chromospheric footpoints along the magnetic field as Alfvénic perturbations. High turbulent velocities above 200 km s?1 can be found around the termination shock, while the low atmosphere reaches turbulent velocities of 10 km s?1 at a layer where the number density is about 1011 cm?3. The turbulent region with maximum nonthermal velocity coincides with the region where the observed high-energy electrons are concentrated, demonstrating the potential role of turbulence in acceleration. Synthetic views in EUV and fitted Hinode-EUV Imaging Spectrometer spectra show excellent agreement with observational results. An energy analysis demonstrates that more than 10% of the reconnection-downflow kinetic energy can be converted to turbulent energy via KHI. |
| 语种 | 英语 |
| 出版者 | The American Astronomical Society |
| WOS记录号 | IOP:APJ_947_2_67 |
| 源URL | [http://ir.iggcas.ac.cn/handle/132A11/110547]  |
| 专题 | 地质与地球物理研究所_中国科学院地球与行星物理重点实验室 |
| 通讯作者 | Ruan,W. |
| 作者单位 | 1.Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, People's Republic of China 2.Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium wenzhi.ruan@kuleuven.be |
| 推荐引用方式 GB/T 7714 | Ruan,W.,Yan,L.,Keppens,R.. Magnetohydrodynamic Turbulence Formation in Solar Flares: 3D Simulation and Synthetic Observations[J]. The Astrophysical Journal,2023,947(2). |
| APA | Ruan,W.,Yan,L.,&Keppens,R..(2023).Magnetohydrodynamic Turbulence Formation in Solar Flares: 3D Simulation and Synthetic Observations.The Astrophysical Journal,947(2). |
| MLA | Ruan,W.,et al."Magnetohydrodynamic Turbulence Formation in Solar Flares: 3D Simulation and Synthetic Observations".The Astrophysical Journal 947.2(2023). |
入库方式： OAI收割
来源：地质与地球物理研究所
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