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 plasma $\beta$ and Alfv\'en Mach number $M_A$ are small and the magnetic field configuration of stationary MHD is basically identical to a nonlinear force-free field, whereas higher up in the corona (where $\beta$ and $M_A$ are above unity) plasma and flow effects become important and stationary MHD and force-free configuration deviate significantly. The new method allows the reconstruction of the coronal magnetic field further outwards than with potential field, nonlinear force-free or magneto-static 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.

中文翻译：

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用太阳风流计算静止 MHD 平衡的优化原理

在这项工作中，我们描述了一种用于计算平稳 MHD 平衡的数值优化方法。新开发的代码基于非线性无力优化原理。我们使用天气矢量磁力图作为边界条件应用我们的代码来模拟日冕。在大约两个太阳半径以下，等离子体 $\beta$ 和 Alfv\'en 马赫数 $M_A$ 很小，并且静止 MHD 的磁场配置基本上与非线性无力场相同，而在日冕更高处（其中$\beta$ 和 $M_A$ 高于统一）等离子体和流动效应变得重要，而固定 MHD 和无力配置显着偏离。与势场、非线性无力或静磁模型相比，新方法允许更向外重建日冕磁场。