太阳大气的磁流体静力学模型通常基于理想化的解析解，因为基本方程太难求解。数值方法，也往往是有限的范围内，往往侧重于二维问题。本文发展了一种求解三维非线性磁流体静力学方程的数值方法。我们的方法是一个固定点迭代计划，扩展了格拉德和鲁宾的方法（Proc.2nd Int.Conf.on Peaceful Uses of Atomic Energy 31，190，1958），包括一个有限的重力。我们将该方法应用到一个测试用例中，以证明该方法的一般性和我们的实现在代码中。
英文摘要：
Magnetohydrostatic models of the solar atmosphere are often based on idealized analytic solutions because the underlying equations are too difficult to solve in full generality. Numerical approaches, too, are often limited in scope and have tended to focus on the two-dimensional problem. In this article we develop a numerical method for solving the nonlinear magnetohydrostatic equations in three dimensions. Our method is a fixed-point iteration scheme that extends the method of Grad and Rubin (Proc. 2nd Int. Conf. on Peaceful Uses of Atomic Energy 31, 190, 1958) to include a finite gravity force. We apply the method to a test case to demonstrate the method in general and our implementation in code in particular.
Analytical Three-dimensional Magnetohydrostatic Equilibrium Solutions for Magnetic Field Extrapolation Allowing a Transition from Non-force-free to Force-free Magnetic Fields
Finite Plasma Beta Three-dimensional Magnetic Field Extrapolation Based on MHD Relaxation Method
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（宇宙科学研究所，日本宇宙航空研究开发机构）；Graduate School of Science, Hiroshima University（广岛大学理学研究院）；Center for Solar-Terrestrial Research, New Jersey Institute of Technology（新泽西理工学院太阳-地球研究中心）
A numerical approach for modelling the polarisation signals of strong resonance lines with partial frequency redistribution. Numerical applications to two-term atoms and plane-parallel atmospheres
