Three-dimensional MHD simulation of the evolution of the April 2000 CME event and its induced shocks using a magnetized plasma blob model
Three-dimensional MHD simulation of the evolution of the April 2000 CME event and its induced shocks using a magnetized plasma blob model
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使用磁化等离子体斑点模型对 2000 年 4 月 CME 事件及其诱发冲击的演化进行三维 MHD 模拟
DOI：
10.1029/2010ja015809
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发表时间：
2011-04
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采用非同步并行时间推进方法，建立了三维时变数值磁流体动力学模型，研究了非均匀背景太阳风中日冕物质抛射的传播。背景太阳风是基于自一致的源面，从2.5 R-s的源面观测到的磁场视距和密度到地球轨道（215 Rs）及更远的地方。日冕物质抛射是通过一个非常简单的通量绳模型来模拟的：一个高密度、高速、高温的磁化等离子体团叠加在一个具有初始发射方向的稳态背景太阳风上。研究了日冕物质抛射与背景太阳风流在2.5 ~ 220 Rs之间的动力学相互作用。研究了与ACE航天器磁连接的碰撞点的物理参数演化。我们选择了2000年4月4-6日的日冕日冕事件作为测试案例。在验证研究中，我们发现采用异步并行时间推进法，以自洽源面为初始边界条件，以简单通量绳为CME模型的三维MHD模型与ACE航天器在L1点的观测结果进行了比较满意的比较。
A three-dimensional (3-D) time-dependent, numerical magnetohydrodynamic (MHD) model with asynchronous and parallel time-marching method is used to investigate the propagation of coronal mass ejections (CMEs) in the nonhomogenous background solar wind flow. The background solar wind is constructed based on the self-consistent source surface with observed line-of-sight of magnetic field and density from the source surface of 2.5 R-s to the Earth's orbit (215 Rs) and beyond. The CMEs are simulated by means of a very simple flux rope model: a high-density, high-velocity, and high-temperature magnetized plasma blob is superimposed on a steady state background solar wind with an initial launch direction. The dynamical interaction of a CME with the background solar wind flow between 2.5 and 220 Rs is investigated. The evolution of the physical parameters at the cobpoint, which is located at the shock front region magnetically connected to ACE spacecraft, is also investigated. We have chosen the well-defined halo-CME event of 4-6 April 2000 as a test case. In this validation study we find that this 3-D MHD model, with the asynchronous and parallel time-marching method, the self-consistent source surface as initial boundary conditions, and the simple flux rope as CME model, provide a relatively satisfactory comparison with the ACE spacecraft observations at the L1 point.
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影响因子：
5.2
作者：
D. McComas;H. Elliott;N. Schwadron;J. Gosling;R. Skoug;Bruce E. Goldstein
通讯作者：
D. McComas;H. Elliott;N. Schwadron;J. Gosling;R. Skoug;Bruce E. Goldstein
影响因子：
2.8
作者：
S. Wu;T. X. Zhang;E. Tandberg-Hanssen;Yang Liu;Xueshang Feng;A. Tan
通讯作者：
S. Wu;T. X. Zhang;E. Tandberg-Hanssen;Yang Liu;Xueshang Feng;A. Tan
小 He2 滑移情况下 MHD Rankine-Hugoniot 关系的新冲击拟合程序
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影响因子：
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作者：
D. Odstrcil;P. Riley;Xuepu Zhao
通讯作者：
D. Odstrcil;P. Riley;Xuepu Zhao
影响因子：
1.5
作者：
S. Plunkett;S. Wu
通讯作者：
S. Plunkett;S. Wu