The infrared Mg I lines near 12 microns are a pair of emission lines which are magnetically sensitive and have been used to measure solar magnetic fields. Here we calculate the response of the Mg I 12.32 $\mu$m line during a flare and find that in our modeling this line has a complicated behavior. At the beginning of the flare heating, this line shows an intensity dimming at the line center. The intensity then increases when heating continues, with increasing contributions from the heated layers in the chromosphere. The line formation height and the line width also increase as a result. As for the polarized line profiles, we find that flare heating tends to decrease the Zeeman splitting width and attenuates the Stokes $V$ lobe intensity. The wider features in the Stokes $V$ profiles are more pronounced during flare heating, which should be considered when performing magnetic field inversions.

中文翻译：

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燃烧大气中 Mg i 12.32 μm 线的非 LTE 计算

接近 12 微米的红外 Mg I 线是一对磁敏感的发射线，已被用于测量太阳磁场。在这里，我们计算了耀斑期间 Mg I 12.32 $\mu$m 线的响应，发现在我们的建模中，这条线具有复杂的行为。在耀斑加热开始时，这条线显示线中心处的强度变暗。当继续加热时，强度会增加，色球中加热层的贡献会增加。结果，线形成高度和线宽也增加。对于极化线轮廓，我们发现耀斑加热倾向于降低塞曼分裂宽度并减弱斯托克斯 $V$ 波瓣强度。Stokes $V$ 剖面中更宽的特征在火炬加热期间更加明显，