论文标题
SI I6560.58Å线的统计分析通过Chase观察到线
Statistical analysis of the Si I 6560.58 Å line observed by CHASE
论文作者
论文摘要
h $α$蓝翼的Si I6560.58Å线与地面观测中的水蒸气的tell尿吸收线混合在一起。对空间望远镜追逐的最新观察为研究这一线提供了一个新的窗口。我们的目标是从统计学上研究SI I系，并探索可能的诊断。我们在追逐观测中选择了三个扫描，并为太阳能磁盘上每个像素的每个像素测量等效宽度（EW）和全宽度。然后，我们从VALC模型中计算理论EW和FWHM。还特别研究了一个活跃的区域，以在宁静的太阳和黑子中差异。 Si I线在光球的底部形成。该线的EW从磁盘中心增加到$μ= 0.2，然后向太阳能肢体减小，而FWHM则显示单调增加的趋势。理论上预测的EW与观察结果很好，而预测的FWHM由于模型中未解决的湍流而少得多。大型速度估计在磁盘中心为2.80 km s $^{ - 1} $，并增加到3.52 km s $^{ - 1} $ at $μ$ = 0.2。在当前观察中，我们没有发现对耀斑加热的任何反应。 Si I6560.58Å和Fe I6569.21Å线的多普勒偏移和线宽度可用于研究不同光平层的质量流和湍流。 Si I系具有良好的潜力，可以诊断光球中的动力和能量传输。
The Si I 6560.58 Å line in the H$α$ blue wing is blended with a telluric absorption line from water vapor in ground-based observations. Recent observations with the space-based telescope CHASE provide a new window to study this line. We aim to study the Si I line statistically and to explore possible diagnostics. We select three scannings in the CHASE observations, and measure the equivalent width (EW) and the full width at half maximum (FWHM) for each pixel on the solar disk. We then calculate the theoretical EW and FWHM from the VALC model. An active region is also studied in particular for difference in the quiet Sun and the sunspots. The Si I line is formed at the bottom of the photosphere. The EW of this line increases from the disk center to $μ$ = 0.2, and then decreases toward the solar limb, while the FWHM shows a monotonically increasing trend. Theoretically predicted EW agrees well with observations, while the predicted FWHM is far smaller due to the absence of unresolved turbulence in models. The macroturbulent velocity is estimated to be 2.80 km s$^{-1}$ at the disk center, and increases to 3.52 km s$^{-1}$ at $μ$ = 0.2. We do not find any response to flare heating in current observations. Doppler shifts and line widths of the Si I 6560.58 Å and Fe I 6569.21 Å lines can be used to study the mass flows and turbulence of the different photospheric layers. The Si I line has good potentials to diagnose the dynamics and energy transport in the photosphere.
