论文标题
Mg I 12.32 $μ$ m线的非LTE计算
Non-LTE Calculations of the Mg I 12.32 $μ$m Line in a Flaring Atmosphere
论文作者
论文摘要
在12微米附近的红外MG I线是一对发射线，在磁性上敏感并已用于测量太阳磁场。在这里，我们计算了耀斑期间Mg I 12.32 $μm线的响应，并发现在我们的建模中，该线的行为具有复杂的行为。在耀斑加热的开头，该线在线中心显示强度变暗。当加热时，强度随着染色体中加热层的贡献增加而增加。线形成的高度和线宽也会增加。至于偏光线轮廓，我们发现火炬加热倾向于降低Zeeman的分裂宽度，并减轻Stokes $ v $叶的强度。在耀斑加热期间，在Stokes $ v $ cob中的更广泛特征更为明显，在执行磁场反演时应考虑这一点。
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 $μ$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.
