Testing magnetohydrostatic extrapolation with radiative MHD simulation of a solar flare
Testing magnetohydrostatic extrapolation with radiative MHD simulation of a solar flare
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DOI：
10.1051/0004-6361/201936433
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发表时间：
2019-10
影响因子：
6.5
通讯作者：
Xiaoshuai Zhu;T. Wiegelmann
中科院分区：
文献类型：
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作者：
Xiaoshuai Zhu;T. Wiegelmann
上下文在太阳上，磁场矢量通常只在光球层中测量。通过使用这些光球测量作为边界条件，我们开发了磁流体静力（MHS）外推模拟太阳大气。该模型假设了磁力和非磁力的相对重要性。虽然日冕是无力的，但光球层和色球层却不是这样。目标。该模型已被测试与精确的平衡。在这里，我们提出了一个更具挑战性和更现实的测试我们的模型与辐射磁流体动力学模拟的太阳耀斑。方法.利用最优化方法，MHS模型自洽地计算了磁场、等离子体压强和密度。以非线性无力场和沿磁力线沿着分布的重力层结大气为初始条件进行优化。结果与NLFFF相比，MHS模型不仅在磁场大小和方向上，而且在磁连通性方面都有所改善。此外，MHS模型还能恢复光球层和色球层等离子体的主要结构。
Context. On the sun, the magnetic field vector is measured routinely solely in the photosphere. By using these photospheric measurements as a boundary condition, we developed magnetohydrostatic (MHS) extrapolation to model the solar atmosphere. The model makes assumptions about the relative importance of magnetic and non-magnetic forces. While the solar corona is force-free, this is not the case with regard to the photosphere and chromosphere. Aims. The model has previously been tested with an exact equilibria. Here we present a more challenging and more realistic test of our model with the radiative magnetohydrodynamic simulation of a solar flare. Methods. By using the optimization method, the MHS model computes the magnetic field, plasma pressure and density self-consistently. The nonlinear force-free field (NLFFF) and gravity-stratified atmosphere along the field line are assumed as the initial conditions for optimization. Results. Compared with the NLFFF, the MHS model provides an improved magnetic field not only in magnitude and direction, but also in magnetic connectivity. In addition, the MHS model is capable of recovering the main structure of plasma in the photosphere and chromosphere.