Nearly all energy generated by fusion in the solar core is ultimately radiated away into space in the solar atmosphere, while the remaining energy is carried away in the form of neutrinos. The exchange of energy between the solar gas and the radiation field is thus an essential ingredient of atmospheric modeling. The equations describing these interactions are known, but their solution is so computationally expensive that they can only be solved in approximate form in multi-dimensional radiation-MHD modeling. In this review, I discuss the most commonly used approximations for energy exchange between gas and radiation in the photosphere, chromosphere, and corona.

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太阳大气模拟中的辐射流体动力学

太阳核中聚变产生的几乎所有能量最终都会被辐射到太阳大气中的太空中，而其余的能量则以中微子的形式被带走。因此，太阳能气体与辐射场之间的能量交换是大气建模的重要组成部分。描述这些相互作用的方程式是已知的，但是它们的解决方案在计算上非常昂贵，以致只能在多维辐射MHD建模中以近似形式求解它们。在这篇评论中，我讨论了光球，色球层和电晕中气体与辐射之间能量交换的最常用近似方法。