Three‐dimensional MHD simulation of two coronal mass ejections' propagation and interaction using a successive magnetized plasma blobs model
Three‐dimensional MHD simulation of two coronal mass ejections' propagation and interaction using a successive magnetized plasma blobs model
复制标题
DOI：
10.1029/2011ja016584
复制
发表时间：
2011-09
影响因子：
--
通讯作者：
F. Shen;X. Feng;Yuming Wang;S. Wu;Wenzhi Song;Jingnan Guo;Yongqiang Zhou
中科院分区：
文献类型：
--
作者：
F. Shen;X. Feng;Yuming Wang;S. Wu;Wenzhi Song;Jingnan Guo;Yongqiang Zhou
利用三维时间相关的数值磁流体动力学（MHD）模型研究了非均匀环境太阳风中两次日冕物质抛射（cme）的演化和相互作用。背景太阳风是在自一致源面基础上构建的，该自一致源面具有观测到的2.5 R(s)至地球轨道（215 R(s)）及以上的磁场视线和密度。选取2001年3月28日连续两次日冕物质抛射并在行星际空间形成多重磁云的日冕物质抛射为试验用例，采用两个高密度、高速、高温磁化等离子体团模型进行模拟，并沿不同初始发射方向先后抛射到非均匀背景太阳风介质中。研究了两个cme在2.5 ~ 220 R(s)范围内的动态传播和相互作用。我们的模拟结果表明，虽然两次CME相隔10 h，但第二次CME能够超过第一次CME并引起复合相互作用和明显的激波加速度。在靠近地球的L1点，我们的模拟结果与ACE的观测结果一致。在验证研究中，我们发现以自洽源面为初始边界条件，磁化等离子体团为CME模型的三维MHD模型能够再现和解释卫星观测到的多重磁云的一些一般特征。
A three-dimensional (3-D), time-dependent, numerical magnetohydrodynamic (MHD) model is used to investigate the evolution and interaction of two coronal mass ejections (CMEs) in the nonhomogeneous ambient solar wind. The background solar wind is constructed on the basis of 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 Earth's orbit (215 R(s)) and beyond. The two successive CMEs occurring on 28 March 2001 and forming a multiple magnetic cloud in interplanetary space are chosen as a test case, in which they are simulated by means of a two high-density, high-velocity, and high-temperature magnetized plasma blobs model, and are successively ejected into the nonhomogeneous background solar wind medium along different initial launch directions. The dynamical propagation and interaction of the two CMEs between 2.5 and 220 R(s) are investigated. Our simulation results show that, although the two CMEs are separated by 10 h, the second CME is able to overtake the first one and cause compound interactions and an obvious acceleration of the shock. At the L1 point near Earth the two resultant magnetic clouds in our simulation are consistent with the observations by ACE. In this validation study we find that this 3-D MHD model, with the self-consistent source surface as the initial boundary condition and the magnetized plasma blob as the CME model, is able to reproduce and explain some of the general characters of the multiple magnetic clouds observed by satellite.