Self Consistent Models of Solar Flare Chromospheres

计划通过发展耀斑中能量传输的自洽模型，为解释硬X射线、软X射线和太阳耀斑的光学观测提供工具。MAX‘91计划正在对当前太阳活动高峰期的耀斑进行前所未有的多波长观测。特别是，计划计算一个物理上自洽的大气模型网格，这些模型处于能量平衡状态，包括非热粒子的能量传输、热传导和所有重要的辐射过程(X射线、紫外线、光学)。完全依赖于时间的模型既不必要也不可取。对于解释观测更有用的是，考虑两种更简单的极限情况：静力极限，通常在几十秒或更长的时间尺度上有效；脉冲极限，其中质量冻结在耀斑前的分布中。为了确定光学厚度色球的加热和冷却，将采用严格的非LTE处理所有重要原子线的辐射转移和统计平衡。这些模型应该为使用综合多波长观测来区分太阳耀斑色球中的热过程和非热过程迈出了重要的一步。

It is planned to provide tools for interpretation of combined hard X-ray, soft X-ray, and optical observations of solar flares by developing self-consistent models of energy transport in flares. The MAX '91 program is providing unprecedented multiwavelength observations of flares during the current solar maximum. In particular, it is planned to compute a grid of physically self-consistent atmospheric models which are in energy balance, including energy transport by nonthermal particles, thermal conduction, and all important radiation processes (X-ray, UV, optical). It is neither necessary or desireable to carry out a fully time-dependent model. It is more useful, for interpretation of the observations to consider two simpler limiting cases: the hydrostatic limit, valid on timescales typically tens of seconds or longer, and the impulsive limit, where the mass is frozen into its preflare distribution. To determine the heating and cooling of the optically thick chromosphere, a rigorous non-LTE treatment of the radiative transfer and statistical equilibrium in all important atomic lines will be employed. These models should provide an important step toward using integrated multi-wavelength observations to discriminate between thermal and nonthermal processes in solar flare chromospheres.