Three‐dimensional MHD simulation of CMEs in three‐dimensional background solar wind with the self‐consistent structure on the source surface as input: Numerical simulation of the January 1997 Sun‐Earth connection event
Three‐dimensional MHD simulation of CMEs in three‐dimensional background solar wind with the self‐consistent structure on the source surface as input: Numerical simulation of the January 1997 Sun‐Earth connection event
复制标题
DOI：
10.1029/2006ja012164
复制
发表时间：
2007-06
影响因子：
--
通讯作者：
F. Shen;Xueshang Feng;S. Wu;C. Xiang
中科院分区：
文献类型：
--
作者：
F. Shen;Xueshang Feng;S. Wu;C. Xiang
利用一个三维时变磁流体动力学（MHD）数值模型研究了日冕物质抛射（CME）在非均匀背景太阳风中的传播。根据太阳磁场和K冕亮度的观测结果，利用MHD方程建立了2.5Rs源面上的自洽结构。利用自洽的源表面结构作为初边值条件，我们开发了一个三维MHD区域组合数值模式程序，以获得从源表面2.5 Rs到地球轨道（215 Rs）及更远的背景太阳风。该模型考虑了太阳自转和体积加热。在内边界处的CME模型配置的压力和速度的时间依赖性变化被应用于生成瞬态结构。研究了2.5 ~ 215 Rs（1 Au）CME与背景太阳风的动力学相互作用。我们选择了1997年1月6日至12日定义明确的晕日冕物质抛射事件作为测试案例。由于在1 Au（风航天器）的这种扰动的详细观测是可用的，这一事件给了我们一个很好的机会来验证我们的MHD方法，并了解太阳地球连接的物理过程。在这项研究中，我们发现，这种三维MHD模型，与自洽结构的源表面作为输入，提供了一个比较令人满意的比较与WIND航天器的观测。
A three-dimensional time-dependent, numerical magnetohydrodynamic (MHD) model is used to investigate the propagation of coronal mass ejections (CMEs) in the nonhomogenous background solar wind flow. On the basis of the observations of the solar magnetic field and K-coronal brightness, the self-consistent structure on the source surface of 2.5 Rs is established with the help of MHD equations. Using the self-consistent source surface structures as initial-boundary conditions, we develop a three-dimensional MHD regional combination numerical model code to obtain the background solar wind from the source surface of 2.5 Rs to the Earth's orbit ( 215 Rs) and beyond. This model considers solar rotation and volumetric heating. Time-dependent variations of the pressure and velocity configured from a CME model at the inner boundary are applied to generate transient structures. The dynamical interaction of a CME with the background solar wind flow between 2.5 and 215 Rs ( 1 AU) is then investigated. We have chosen the well-defined halo-CME event of 6 - 12 January 1997 as a test case. Because detailed observations of this disturbance at 1 AU ( by WIND spacecraft) are available, this event gives us an excellent opportunity to verify our MHD methodology and to learn about the physical processes of the Sun-Earth connection. In this study, we find that this three-dimensional MHD model, with the self-consistent structures on the source surface as input, provides a relatively satisfactory comparison with the WIND spacecraft observations.