An Optimization Principle for Computing Stationary MHD Equilibria with Solar Wind Flow
An Optimization Principle for Computing Stationary MHD Equilibria with Solar Wind Flow
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DOI：
10.1007/s11207-020-01719-8
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发表时间：
2020-03
期刊：
影响因子：
2.8
通讯作者：
T. Wiegelmann;T. Neukirch;D. Nickeler;I. Chifu
中科院分区：
文献类型：
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作者：
T. Wiegelmann;T. Neukirch;D. Nickeler;I. Chifu
在这项工作中，我们描述了一个数值优化方法计算固定MHD平衡。新开发的代码是基于非线性力自由优化原理。我们使用天气矢量磁图作为边界条件来模拟日冕。在大约两个太阳半径以下，等离子体和阿尔文马赫数都很小，稳态MHD的磁场结构基本上与非线性无力场相同，而在日冕更高的地方（和大于1），等离子体和流动效应变得很重要，稳态MHD和无力结构偏离很大。与势场、非线性无力或静磁模型相比，新方法可以更向外地重建日冕磁场。该模型可为太阳轨道器和帕克太阳探测器上的遥感和现场仪器的联合观测提供磁连通性。
In this work we describe a numerical optimization method for computing stationary MHD equilibria. The newly developed code is based on a nonlinear force-free optimization principle. We apply our code to model the solar corona using synoptic vector magnetograms as boundary condition. Below about two solar radii the plasmaand Alfvén Mach numberare small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (whereandare above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows for the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magnetostatic models. This way the model might help to provide the magnetic connectivity for joint observations of remote sensing and in-situ instruments on Solar Orbiter and Parker Solar Probe.