2.5维自适应磁场重联MHD模式

张绍华; 冯学尚; 杨利平

doi:10.11728/cjss2012.06.785

2.5维自适应磁场重联MHD模式

doi: 10.11728/cjss2012.06.785

1.
中国科学院空间科学与应用研究中心空间天气学国家重点实验室北京 100190
2.
中国科学院大学北京 100049

基金项目: 国家自然科学基金项目(41031066, 40921063, 40874091, 40890162, 41074122)和空间天气学国家重点实验室专项基金共同资助

详细信息

中图分类号: P353
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出版历程
- 收稿日期: 2011-05-26
- 修回日期: 2012-05-03
- 刊出日期: 2012-11-15

2.5D AMR MHD Magnetic Reconnection Model

1.
State Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100190
2.
University of Chinese Academy of Sciences, Beijing 100049

摘要

摘要: 磁雷诺数(R_m)是影响磁场重联的重要因素. 真实的物理环境中R_m往往很高, 例如, 在行星际空间和太阳日冕中R_m通常大于10⁴量级. 高R_m条件下的磁重联表现出很多异常特性, 然而高R_m条件下的磁场重联数值模拟需要很高的时空分辨率, 否则很难分辨出重联过程中形成的薄电流片. 本文基于自适应软件包PARAMESH将并行自适应网格技术引入磁场重联数值模拟, 建立了一个2.5维自适应磁场重联MHD模式, 研究高磁雷诺数条件下重联的动态演化过程, 进而将不同磁雷诺数的参数进行对比研究. 结果表明, 该模式可以自动捕捉到磁场重联产生的奇性电流片, 高磁雷诺数条件下产生的慢激波结构可提供一种快速磁能释放机制.
- 自适应 /
- 磁场重联 /
- MHD数值模拟
Abstract: Magnetic reconnection is one of the hot topics in space physics. The magnetic Lundquist number can influence the magnetic reconnection process drastically. Magnetic Lundquist number is always very large in many real physical environments, for example, higher than 10⁴ in interplanetary space and solar corona. Magnetic reconnection with enormously large Lundquist number behaves many new characteristics, while magnetic reconnection simulation needs very high grid resolution, or it can't resolve the thin current sheets formed in the magnetic reconnection. With the help of the Adaptive Mesh Refinement (AMR) package named PARAMESH, AMR technique was introduced into magnetic reconnection simulations and a two and half dimensional (2.5D) AMR magnetic reconnection model was developed. The dynamic reconnection process with different magnetic Lundquist numbers was studied. The results showed that this model can automatically capture the near-singular current sheets with the development of the magnetic reconnection and the slow-mode shock structures formed in the magnetic reconnection process with high magnetic Lundquist number provide a possible way for fast magnetic energy conversion.
- AMR /
- Magnetic reconstruction /
- MHD simulation

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参考文献(28)

[1]	Aschwanden M J. Particle acceleration and kinematics in solar flares-A synthesis of recent observations and theoretical concepts[J]. Space Sci. Rev., 2002, 101:1-227
[2]	Birn J, Priest E R. Magnetohydrodynamics and Collisionless Theory and Observations[M]. Cambridge: Cambridge University Press, 2006
[3]	Wei Fengsi, Schwenn R, Hu Qiang. Magnetic reconnection events in the interplanetary space[J]. Sci. China E: Tech. Sci., 1997, 40:463-471
[4]	Wei Fengsi, Hu Qiang, Feng Xueshang, Fan Quanlin. Magnetic reconnection phenomena in interplanetary space[J]. Space Sci. Rev., 2003, 107:107-110
[5]	Ugai M. Basic physical mechanism of fast reconnection evolution in space plasmas[J]. Space Sci. Rev., 2001, 95:601-611
[6]	Litvinenko Y E. Particle acceleration in reconnecting current sheets in impulsive electron-rich solar flares[J]. Solar Phys., 2000, 194:327-343
[7]	Litvinenko Y E. Electron acceleration in solar flares[J]. Adv. Space Res., 2003, 32:2385-2391
[8]	Gordovskyy M, Browning P K, Vekstein G E. Particle acceleration in fragmenting periodic reconnecting current sheets in solar flares[J]. Astrophys. J., 2010, 720:1603-1611
[9]	Fu X R, Lu Q M, Wang S. The process of electron acceleration during collisionless magnetic reconnection[J]. Phys. Plasmas, 2006, 13:1-8
[10]	Huang C, Lu Q M, Wang S. The mechanisms of electron acceleration in antiparallel and guide field magnetic reconnection[J]. Phys. Plasmas, 2010, 17:1-8
[11]	Priest E R, Forbes T G. The magnetic nature of solar flares[J]. Astron. Astrophys. Rev., 2002, 10:313-377
[12]	Cassak P A, Shay M A. Magnetic reconnection for coronal conditions: reconnection rates, secondary islands and onset[J]. Space Sci. Rev., 2011, 11:1-20
[13]	Wei Fengsi, Hu Qiang, Feng Xueshang. Numerical study of magnetic reconnection process near interplanetary current sheet[J]. Chin. Sci. Bull., 2001, 46:111-117
[14]	Barta M, Buchner J, Karlicky M. Multi-scale MHD approach to the current sheet filamentation in solar coronal reconnection[J]. Adv. Space Res., 2010, 45:10-17
[15]	Berger M J, Oliger J. Adaptive mesh refinement for hyperbolic partial differential equations[J]. J. Comput. Phys., 1984, 53:484-512
[16]	Barta M, Buchner J, Karlicky M. Spontaneous current-layer fragmentation and cascading reconnection in solar flares: II Relation to observations[J]. Astrophys. J., 2011, 47:1-6
[17]	Loureiro N F, Schekochihin A A, Cowley S C. Instability of current sheets and formation of plasmoid chains[J]. Phys. Plasmas, 2007, 14:100703-100707
[18]	Samtaney R, Loureiro N F, Uzdensky D A, Schekochihin A A, Cowley S C. Formation of plasmoid chains in magnetic reconnection[J]. Phys. Rev. Lett., 2009, 103:1-4
[19]	Huang Y M, Bhattacharjee A. Scaling laws of resistive magnetohydrodynamic reconnection in the high-Lundquist-number, plasmoid-unstable regime[J]. Phys. Plasmas, 2010, 17:062104-062111
[20]	Wang R S, Du A M, Wang S. In-situ observations of a secondary magnetic island in an ion diffusion region and associated energetic electrons[J]. Phys. Rev. Lett., 2010, 104:1-4
[21]	Li Xing, Huang C. Observations of energetic electrons up to 200keV associated with a secondary island near the center of an ion diffusion region: A Cluster case study[J]. J. Geophys. Res., 2010, 115:1-10
[22]	Kurganov A, Noelle S, Petrova G. Semidiscrete central-upwind schemes for hyperbolic conservation laws and hamilton-jacobi equations[J]. SIAM J. Sci. Comput., 2001, 23:707-740
[23]	Ziegler U. A central-constrained transport scheme for ideal magnetohydrodunamics[J]. J. Comput. phys., 2004, 196:393-416
[24]	Toth G. The abla · ±b B = 0 constraint in shock-capturing magnetohydrodynamics codes[J]. J. Comput. Phys., 2000, 161:605-652
[25]	Wang Y, Wei F S, Feng X S, Zhang S H, Zuo P B, Sun T R. Energetic electrons associated with magnetic reconnection in the magnetic cloud boundary layer[J]. Phys. Rev. Lett., 2010, 105:1-4
[26]	Birn J, Drake J F, Shay M A. Geospace Environmental Modeling (GEM) magnetic reconnection challenge[J]. J. Geophys. Res., 2001, 106:3715-3720
[27]	Loureiro N F, Cowley S C, Dorland W D, Haines M G, Schekochihin A A. X-point collapse and saturation in the nonlinear tearing mode reconnection [J]. Phys. Rev. Lett., 2005, 95:1-4
[28]	Oka M, Phan T D, Krucker S, Fujimoto M, Shinohara I. Electron acceleration by multi-Island coalescence[J]. Astrophys. J., 2010, 714:915-926