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.

太阳核心聚变产生的几乎所有能量最终都会辐射到太阳大气中的太空中，而剩余的能量则以中微子的形式被带走。因此，太阳气体和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是已知的，但它们的解在计算上非常昂贵，以至于它们只能在多维辐射 MHD 建模中以近似形式求解。在这篇综述中，我讨论了光球层、色球层和日冕中气体和辐射之间能量交换最常用的近似值。