太阳大气中的非等温静磁平衡结构

NON-ISOTHERMAL MAGNETOHYDROSTATIC EQUILIBRIUM STRUCTURE IN THE SOLAR ATMOSPHERE

本文以等温静磁平衡结构的解为基础,进一步研究非等温情况的静磁平衡结构.并考虑两种温度分布模型,导出与这两种情况对应的静磁平衡所满足的偏微分方程.用等温解作为一级近似函数值,选择适当的边界条件,用迭代法求得它们的数值解.文中还给出这两种模型的非等温静磁平衡结构位形图,温度分布图及磁能分布图.分析研究这些分布,我们发现:微小的温度梯度将使平衡结构位形有明显的变化.温度的变化可能导致不稳定性,从而引起比较剧烈的太阳活动.

The non-isothermal magnetohydrostatic equilibrium is studied in this paper. On the basis of two-dimensional solutions of an isothermal case [9]. We present two models of temperature distribution and derive the two relevant partial differential equations of non-isothermal magnetohydrostatic equilibrium. Using the solution of the isothermal case as an approximation of the 1st degree and choosing appropriate boundary conditions, we obtain several solutions of the equations with an iterative method numerically, and obtain the equilibrium configurations and the distributions of temperature and magnetic energy. From these results, we find that the equilibrium configurations will change obviously as the temperature changes from the isothermal case slightly. Change of the temperature may play an important role in producing relatively violent solar activities through instability.