-
近20年来, 大量的磁岛链现象从空间、天体物理到磁约束实验室等离子体中被观察到, 并且有关磁岛链现象的许多物理特性可以直接被计算机模拟结果所证实. 磁岛链理论在磁重联理论中的重要进展为快速磁重联的发生机制提供了更加具有说服力的解释. 本文采用二维三分量的磁流体力学模型, 数值研究了不同宽度和不同强度的垂直平面驱动流对磁重联中磁岛链不稳定性的影响, 并分析了导向场和垂直平面的驱动流对磁岛链的共同作用. 研究结果表明: 垂直平面驱动流的宽度越宽或强度越强, 越容易产生磁岛链结构. 电流片中的小磁岛个数及重联率随着垂直平面驱动流宽度及强度的增加而增加. 另外, 导向场会改变重联平面内磁岛链的对称性. 相同导向场情况下, 驱动流强度越大, 小磁岛的增长速度越快.In the last two decades, a wide variety of plasmoids events have been observed, ranging from space and astrophysical phenomenon to magnetically confined laboratory plasmas, in which there are a lot of evidence of observational plasmoid-like features supported by direct large-scaled computer simulations. A super-Alfvénic instability, named plasmoid instability, occurs in an extended current sheet, when the Lundquist number exceeds a critical value. The large-aspect-ratio current sheet is fragmented by generating, growing, coalescing and ejecting of plasmoids so that this phenomenon has been proposed as a possible mechanism for fast reconnection scenario. This super-Alfvénic plasmoid instability has been usedin the significant new development of reconnection theory, and thus can provide alternative and more convincing mechanism for fast reconnection. In this work, a “driving” kind of shear flow in the out-of-plane direction is imposed on a two-dimensional, three-component magnetohydrodynamic model with a current sheet system to study the dynamic process of the plasmoids in a current sheet system. The effect of the width and strength of the driving flow on the reconnection rate of plasmoids are numerically analyzed in detail. It is found that the plasmoids are easily formed in the case of strong and wide out-of-plane driving flow. The reconnection rate and the number of the plasmoids increase with the driving flow width and/or driving flow strength increasing. In the presence of guiding field, it is found that the symmetry of the plasmoids is broken in the reconnection plane. In addition, for the fixed guiding field, the growth rate of plasmoids increases much faster when the strength of driving flow increases.
-
Keywords:
- magnetic reconnection /
- plasma driving flow /
- plasmiods /
- guiding field
[1] Parker E N 1963 Astrophys. J. Suppl. Ser. 8 177
Google Scholar
[2] Sweet P A 1969 Annu. Rev. Astron. Astr. 7 149
Google Scholar
[3] Yokoyama T, Akita K, Morimoto T, Inoue K, Newmark J 2001 Astrophys. J. Lett. 546 L69
Google Scholar
[4] Dungey J W 1961 Phys. Rev. Lett. 6 47
Google Scholar
[5] Bhattacharjee A 2004 Annu. Rev. Astron. Astr. 42 365
Google Scholar
[6] Hastie R J 1997 Astrophys. Space Sci. 256 177
Google Scholar
[7] Chapman I T, Scannell R, Cooper W A, Graves J P, Hastie R J, Naylor G, Zocco A 2010 Phys. Rev. Lett. 105 255002
Google Scholar
[8] Wei L, Wang Z X, Fan D M, Wang F, Liu Y 2011 Phys. Plasmas 18 042503
Google Scholar
[9] Zhang C L, Ma Z W 2009 Phys. Plasmas 16 122113
Google Scholar
[10] Jin S P, Yang H A, Wang X G 2005 Phys. Plasmas 12 042902
Google Scholar
[11] Ishizawa A, Waelbroeck F L, Fitzpatrick R, Horton W, Nakajima N 2012 Phys. Plasmas 19 072312
Google Scholar
[12] Biskamp D 1986 Phys. Fluids. 29 1520
Google Scholar
[13] Daughton W, Scudder J, Karimabadi H 2006 Phys. Plasmas 13 072101
Google Scholar
[14] Drake J F, Swisdak M, Che H, Shay M A 2006 Nature 443 553
Google Scholar
[15] Loureiro N F, Schekochihin A A, Cowley S C 2007 Phys. Plasmas 14 100703
[16] Lapenta G 2008 Phys. Rev. Lett. 100 235001
Google Scholar
[17] Lin J, Cranmer S R, Farrugia C J 2008 J. Geophys. Res. 113 D11107
Google Scholar
[18] Bhattacharjee A, Huang Y M, Yang H, Rogers B 2009 Phys. Plasmas 16 112102
Google Scholar
[19] Daughton W, Roytershteyn V, Albright B J, Karimabadi H, Yin L, Bowers K J 2009 Phys. Rev. Lett. 103 065004
Google Scholar
[20] Huang Y M, Bhattacharjee A, Sullivan B P 2011 Phys. Plasmas 18 072109
Google Scholar
[21] Nemati M J, Wang Z X, Wei L, Selim B I 2015 Phys. Plasmas 22 012106
Google Scholar
[22] Samtaney R, Loureiro N F, Uzdensky D A, Schekochihin A A, Cowley S C 2009 Phys. Rev. Lett. 103 105004
Google Scholar
[23] Pritchett P L, Lee Y C, Drake J F 1980 Phys. Fluids 23 1368
Google Scholar
[24] Ishii Y, Azumi M, Kishimoto Y 2002 Phys. Rev. Lett. 89 205002
Google Scholar
[25] Wang Z X, Wang X, Dong J Q, Kishimoto Y, Li J Q 2008 Phys. Plasmas 15 082109
Google Scholar
[26] Wang Z X, Wang X G, Dong J Q, Lei Y A, Long Y X, Mou Z Z, Qu W X 2007 Phys. Rev. Lett. 99 185004
Google Scholar
[27] Bierwage A, Hamaguchi S, Wakatani M, Benkadda S, Leoncini X 2005 Phys. Rev. Lett. 94 065001
Google Scholar
[28] Bowers K, Li H 2007 Phys. Rev. Lett. 98 035002
Google Scholar
[29] Nemati M J, Wang Z X, Wei L 2016 Astrophys. J. 821 128
Google Scholar
[30] Nemati M J, Wang Z X, Wei L 2017 Astrophys. J. 835 191
Google Scholar
[31] La BelleHamer A L, Otto A, Lee L C 1994 Phys. Plasmas 1 706
Google Scholar
[32] Wang J, Xiao C, Wang X 2012 Phys. Plasmas 19 032905
Google Scholar
[33] Wang L, Wang X Q, Wang X G, Liu Y 2014 Chin. Phys. B 23 025203
Google Scholar
-
图 2 无驱动流情况下的磁岛位型 (a), (b), (c), (d)分别为时间t = 70, t = 74, t = 80和t = 120的结构, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度
Fig. 2. The magnetic configuration without driving flow at (a) t = 70, (b) t = 74, (c) t = 80, (d) t = 120. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respectively.
图 3 加入宽度LS = 0.05、强度U0 = 0.1的驱动流时, 磁岛链的演化过程 (a), (b), (c)分别为时间t = 70, t = 80和t = 110的结构, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度
Fig. 3. Evolution of magnetic configuration with out-of-plane driving flow for LS = 0.05, U0 = 0.1 at (a) t = 70, (b) t = 80, (c) t = 110. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respec-tively.
图 4 加入宽度LS = 0.3, 强度U0 = 0.1 驱动流情况下的磁岛位型 (a), (b), (c)为时间t = 80, t = 110和t = 118的结构, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度
Fig. 4. The magnetic configuration with out-of-plane dri-ving flow for LS = 0.3, U0 = 0.1 at (a) t = 80, (b) t = 110, (c) t = 118. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respectively.
图 5 相同宽度LS = 0.3, 不同强度的驱动流, 重联通量随时间的演化
Fig. 5. The evolution of reconnected flux with different driving flow strength.
图 6 加入相同宽度LS = 0.3, 不同强度的驱动流时的典型磁岛位型, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度 (a)无驱动流的情况t = 120的结构; (b)加入强度U0 = 0.1的情况在t = 118的结构; (c)加入强度U0 = 0.2的情况在t = 97的结构; (d)加入强度U0 = 0.3的情况在t = 88的结构
Fig. 6. The magnetic configuration with out-of-plane dri-ving flow with different strength for LS = 0.3 in the same phase. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respectively: (a) Without driving flow at t = 120; (b) with U0 = 0.1 at t = 118; (c) with U0 = 0.2 at t = 97; (d) with U0 = 0.3 at t = 88.
图 7 导向场By = 0.1, 驱动流宽度LS = 0.05、强度U0 = 0.1情况下的磁岛位型 (a), (b), (c)分别为时间t = 100, t = 110和t = 119的结构, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度
Fig. 7. The magnetic configuration is effected by out-of-plane driving flow with LS = 0.05, U0 = 0.1 and guilding field By = 0.1 at (a) t = 100, (b) t = 110, (c) t = 119. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respectively.
图 8 驱动流宽度LS = 0.3, 强度U0 = 0.1, 导向场By = 0.1的情况下, 磁岛位形的演化 (a), (b), (c)分别为时间t = 70, t = 80和t = 88的结构, 黑线和背景颜色分别为重联平面的磁力线分布和垂直平面的电流密度
Fig. 8. Evolution of the magnetic configuration with out-of-plane driving flow for LS = 0.3, U0 = 0.1 and guilding field By = 0.1 at (a) t = 70; (b) t = 80; (c) t = 88. The black lines and background colors indicate the magnetic field line in the reconnection plane and the current density in out-of-plane direction, respectively.
图 9 (a)驱动流宽度LS = 0.05, 强度U0 = 0.1时, 不同导向场By重联通量随时间的演化; (b)导向场By = 0.1, 驱动流宽度LS = 0.05时, 不同强度U0下重联通量随时间的演化; (c)导向场By = 0.1, 驱动流宽度LS = 0.05时, 小磁岛宽度的增长速度对强度U0的依赖关系
Fig. 9. (a) Evolution of the reconnection flux with out-of-plane driving flow for LS = 0.05, U0 = 0.1 and different guilding field; (b) evolution of the reconnection flux with different driving flow strength and guilding field By = 0.1; (c) dependence of the growth rate of plasmoid on different driving flow strength with guilding field By = 0.1.
-
[1] Parker E N 1963 Astrophys. J. Suppl. Ser. 8 177
Google Scholar
[2] Sweet P A 1969 Annu. Rev. Astron. Astr. 7 149
Google Scholar
[3] Yokoyama T, Akita K, Morimoto T, Inoue K, Newmark J 2001 Astrophys. J. Lett. 546 L69
Google Scholar
[4] Dungey J W 1961 Phys. Rev. Lett. 6 47
Google Scholar
[5] Bhattacharjee A 2004 Annu. Rev. Astron. Astr. 42 365
Google Scholar
[6] Hastie R J 1997 Astrophys. Space Sci. 256 177
Google Scholar
[7] Chapman I T, Scannell R, Cooper W A, Graves J P, Hastie R J, Naylor G, Zocco A 2010 Phys. Rev. Lett. 105 255002
Google Scholar
[8] Wei L, Wang Z X, Fan D M, Wang F, Liu Y 2011 Phys. Plasmas 18 042503
Google Scholar
[9] Zhang C L, Ma Z W 2009 Phys. Plasmas 16 122113
Google Scholar
[10] Jin S P, Yang H A, Wang X G 2005 Phys. Plasmas 12 042902
Google Scholar
[11] Ishizawa A, Waelbroeck F L, Fitzpatrick R, Horton W, Nakajima N 2012 Phys. Plasmas 19 072312
Google Scholar
[12] Biskamp D 1986 Phys. Fluids. 29 1520
Google Scholar
[13] Daughton W, Scudder J, Karimabadi H 2006 Phys. Plasmas 13 072101
Google Scholar
[14] Drake J F, Swisdak M, Che H, Shay M A 2006 Nature 443 553
Google Scholar
[15] Loureiro N F, Schekochihin A A, Cowley S C 2007 Phys. Plasmas 14 100703
[16] Lapenta G 2008 Phys. Rev. Lett. 100 235001
Google Scholar
[17] Lin J, Cranmer S R, Farrugia C J 2008 J. Geophys. Res. 113 D11107
Google Scholar
[18] Bhattacharjee A, Huang Y M, Yang H, Rogers B 2009 Phys. Plasmas 16 112102
Google Scholar
[19] Daughton W, Roytershteyn V, Albright B J, Karimabadi H, Yin L, Bowers K J 2009 Phys. Rev. Lett. 103 065004
Google Scholar
[20] Huang Y M, Bhattacharjee A, Sullivan B P 2011 Phys. Plasmas 18 072109
Google Scholar
[21] Nemati M J, Wang Z X, Wei L, Selim B I 2015 Phys. Plasmas 22 012106
Google Scholar
[22] Samtaney R, Loureiro N F, Uzdensky D A, Schekochihin A A, Cowley S C 2009 Phys. Rev. Lett. 103 105004
Google Scholar
[23] Pritchett P L, Lee Y C, Drake J F 1980 Phys. Fluids 23 1368
Google Scholar
[24] Ishii Y, Azumi M, Kishimoto Y 2002 Phys. Rev. Lett. 89 205002
Google Scholar
[25] Wang Z X, Wang X, Dong J Q, Kishimoto Y, Li J Q 2008 Phys. Plasmas 15 082109
Google Scholar
[26] Wang Z X, Wang X G, Dong J Q, Lei Y A, Long Y X, Mou Z Z, Qu W X 2007 Phys. Rev. Lett. 99 185004
Google Scholar
[27] Bierwage A, Hamaguchi S, Wakatani M, Benkadda S, Leoncini X 2005 Phys. Rev. Lett. 94 065001
Google Scholar
[28] Bowers K, Li H 2007 Phys. Rev. Lett. 98 035002
Google Scholar
[29] Nemati M J, Wang Z X, Wei L 2016 Astrophys. J. 821 128
Google Scholar
[30] Nemati M J, Wang Z X, Wei L 2017 Astrophys. J. 835 191
Google Scholar
[31] La BelleHamer A L, Otto A, Lee L C 1994 Phys. Plasmas 1 706
Google Scholar
[32] Wang J, Xiao C, Wang X 2012 Phys. Plasmas 19 032905
Google Scholar
[33] Wang L, Wang X Q, Wang X G, Liu Y 2014 Chin. Phys. B 23 025203
Google Scholar
-
[1] 杨振宇, 张元哲, 范威, 杨广杰, 韩先伟. 磁等离子体发动机中磁喷管分离过程的流体模拟. 物理学报, 2024, 73(10): 105201. doi: 10.7498/aps.73.20231862 [2] . 磁约束等离子体中的高能量粒子专题编者按. 物理学报, 2023, 72(21): 210101. doi: 10.7498/aps.72.210101 [3] 周利娜, 胡汉卿, 刘钺强, 段萍, 陈龙, 张瀚予. 等离子体对共振磁扰动的流体和动理学响应的模拟研究. 物理学报, 2023, 72(7): 075202. doi: 10.7498/aps.72.20222196 [4] 苏祥, 王先驱, 符添, 许宇鸿. CFQS准环对称仿星器低 $\boldsymbol \beta$ 等离子体中三维磁岛的抑制机制. 物理学报, 2023, 72(21): 215205. doi: 10.7498/aps.72.20230546[5] 满良, 邓浩川, 吴洋, 余西龙, 肖志河. 风洞模拟等离子体绕流场回波频谱调制特性实验研究. 物理学报, 2022, 71(3): 035203. doi: 10.7498/aps.71.20211471 [6] 陈国华, 石科军, 储进科, 吴昊, 周池楼, 肖舒. 环形磁场金属等离子体源冷却流场的数值模拟与优化. 物理学报, 2021, 70(7): 075203. doi: 10.7498/aps.70.20201368 [7] 满良, 邓浩川. 风洞模拟等离子体绕流场回波频谱调制特性实验研究. 物理学报, 2021, (): . doi: 10.7498/aps.70.20211471 [8] 苏春燕, 牟茂淋, 陈少永, 郭文平, 唐昌建. 托卡马克等离子体中共振磁扰动场放大效应对离子轨道特性的作用. 物理学报, 2021, 70(9): 095207. doi: 10.7498/aps.70.20201860 [9] 于家成, 仲佳勇, 安维明, 平永利. 短脉冲强激光驱动磁重联过程的靶后电势分布特征. 物理学报, 2021, 70(6): 065201. doi: 10.7498/aps.70.20201339 [10] 原晓霞, 仲佳勇. 双等离子体团相互作用的磁流体力学模拟. 物理学报, 2017, 66(7): 075202. doi: 10.7498/aps.66.075202 [11] 张凯, 仲佳勇, 裴晓星, 李玉同, 阪和洋一, 魏会冈, 袁大伟, 李芳, 韩波, 王琛, 贺昊, 尹传磊, 廖国前, 方远, 杨骕, 远晓辉, 梁贵云, 王菲鹿, 朱健强, 丁永坤, 张杰, 赵刚. 激光驱动磁重联过程中的喷流演化和电子能谱测量. 物理学报, 2015, 64(16): 165201. doi: 10.7498/aps.64.165201 [12] 胡明, 万树德, 钟雷, 刘昊, 汪海. 磁控直流辉光等离子体放电特性. 物理学报, 2012, 61(4): 045201. doi: 10.7498/aps.61.045201 [13] 刘惠平, 邹秀, 邹滨雁, 邱明辉. 电负性等离子体磁鞘的玻姆判据. 物理学报, 2012, 61(3): 035201. doi: 10.7498/aps.61.035201 [14] 李钢, 李轶明, 徐燕骥, 张翼, 李汉明, 聂超群, 朱俊强. 介质阻挡放电等离子体对近壁区流场的控制的实验研究. 物理学报, 2009, 58(6): 4026-4033. doi: 10.7498/aps.58.4026 [15] 郑永真, 齐昌炜, 丁玄同, 郦文忠. 托卡马克等离子体中内部磁扰动的测量研究. 物理学报, 2006, 55(1): 294-298. doi: 10.7498/aps.55.294 [16] 吴成, 叶茂福, 张宝珍, 李银安. 反场角收缩等离子体的压缩和捕获磁通. 物理学报, 1987, 36(9): 1105-1111. doi: 10.7498/aps.36.1105 [17] 董家齐. 有磁辫等离子体的双撕裂模研究. 物理学报, 1984, 33(10): 1341-1349. doi: 10.7498/aps.33.1341 [18] 李家全. 磁阱中的低温等离子体. 物理学报, 1980, 29(11): 1471-1478. doi: 10.7498/aps.29.1471 [19] 石长和. 不均匀等离子体片流的磁流不稳定性. 物理学报, 1979, 28(2): 263-267. doi: 10.7498/aps.28.263 [20] 石长和. 磁流波在部分电离等离子体内的传播. 物理学报, 1965, 21(1): 227-230. doi: 10.7498/aps.21.227
下载:
计量
- 文章访问数: 6357
- PDF下载量: 73
- 被引次数: 0
