THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID
复制标题
通过具有六分量网格的 SIP-CES MHD 模型对从太阳到地球的三维太阳风进行建模
DOI：
10.1088/0004-637x/723/1/300
复制
发表时间：
2010-11-01
影响因子：
4.9
通讯作者：
Zhong, DingKun
中科院分区：
文献类型：
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作者：
Feng, Xueshang;Yang, Liping;Zhong, DingKun
本文的目的是利用三维（3D）太阳-行星际守恒元/解元MHD模型，探讨六分量重叠网格在太阳风模拟中的应用。我们的数值模型的基本重点是致力于处理：(1)利用六分量网格系统求解极点附近的奇异性和网格收敛；(2)利用快速多网格泊松求解器求解易于使用的∇·B约束误差；(3)利用Courant-Friedrichs-Levy数不敏感方法求解Courant-Friedrichs-Levy数视差；(4)利用多次时间步进求解时间积分；(5)利用限制太阳表面逃逸的质量通量求解亚音速区域的时间依赖边界条件。为了产生太阳风的快速和慢速等离子体流，我们通过涉及磁场膨胀因子fS的拓扑效应和开放场脚点与其最近的日冕洞边界之间的最小角距离θb（在光球上），包括体积加热源项和动量加法。这些考虑可以帮助我们方便地对现有程序进行编码，方便地进行并行实现，有效地缩短计算时间，大大提高数值解的精度，合理地产生结构化太阳风。本文以卡林顿旋转1911从太阳到地球的三维稳态背景太阳风数值研究为例，说明了上述优点。我们的数值结果表明，在太阳和日球层观测卫星上的大角度和光谱日冕仪和1 AU的WIND观测在太阳日冕上的总体一致性很好。
The objective of this paper is to explore the application of a six-component overset grid to solar wind simulation with a three-dimensional (3D) Solar-InterPlanetary Conservation Element/Solution Element MHD model. The essential focus of our numerical model is devoted to dealing with: (1) the singularity and mesh convergence near the poles via the use of the six-component grid system, (2) the ∇ · B constraint error via an easy-to-use cleaning procedure by a fast multigrid Poisson solver, (3) the Courant–Friedrichs–Levy number disparity via the Courant-number insensitive method, (4) the time integration by multiple time stepping, and (5) the time-dependent boundary condition at the subsonic region by limiting the mass flux escaping through the solar surface. In order to produce fast and slow plasma streams of the solar wind, we include the volumetric heating source terms and momentum addition by involving the topological effect of the magnetic field expansion factor fS and the minimum angular distance θb (at the photosphere) between an open field foot point and its nearest coronal hole boundary. These considerations can help us easily code the existing program, conveniently carry out the parallel implementation, efficiently shorten the computation time, greatly enhance the accuracy of the numerical solution, and reasonably produce the structured solar wind. The numerical study for the 3D steady-state background solar wind during Carrington rotation 1911 from the Sun to Earth is chosen to show the above-mentioned merits. Our numerical results have demonstrated overall good agreements in the solar corona with the Large Angle and Spectrometric Coronagraph on board the Solar and Heliospheric Observatory satellite and at 1 AU with WIND observations.