与其它强夫琅和费谱线相比，NaI D1中的静太阳成像不对称性
Quiet-Sun imaging asymmetries in NaI D1 compared with other strong Fraunhofer lines
摘要：
使用NaI D1线的太阳大气成像光谱在蓝翼和红线翼之间产生明显的不对称性：在蓝翼中对安静的太阳区域进行采样显示反向颗粒化，而在红翼中进行采样显示正常颗粒化。强度相当的MgI b2线没有显示这种不对称性，更强的CaII 8542线也没有。我们证明了这一现象与近同时光谱图像NaI D1，MgI B2，和CaII 8542从瑞典1米太阳望远镜。然后，我们解释它与线形成的见解，从经典的1D建模和3D磁流体动力学模拟结合NLTE谱线合成，允许详细的比较，在一个共同的格式的意见。成像不对称的原因是粒度过冲中的强度和多普勒频移调制之间的相关性以及对NaI D1线的陡峭轮廓侧翼的敏感性的组合。MgI b2线有类似的核心形成，但更广泛的翅膀，由于更大的不透明度建设和光球阻尼。这两条线获得显着的核心不对称性光球冲击或附近的强磁浓度，更高的网络间的冲击，产生类似的不对称性，在空间平均的CaII 8542配置文件。
英文摘要：
Imaging spectroscopy of the solar atmosphere using the NaI D1 line yields marked asymmetry between the blue and red line wings: sampling a quiet-Sun area in the blue wing displays reversed granulation, whereas sampling in the red wing displays normal granulation. The MgI b2 line of comparable strength does not show this asymmetry, nor does the stronger CaII 8542 line. We demonstrate the phenomenon with near-simultaneous spectral images in NaI D1, MgI b2, and CaII 8542 from the Swedish 1-m Solar Telescope. We then explain it with line-formation insights from classical 1D modeling and with a 3D magnetohydrodynamical simulation combined with NLTE spectral line synthesis that permits detailed comparison with the observations in a common format. The cause of the imaging asymmetry is the combination of correlations between intensity and Dopplershift modulation in granular overshoot and the sensitivity to these of the steep profile flanks of the NaI D1 line. The MgI b2 line has similar core formation but much wider wings due to larger opacity buildup and damping in the photosphere. Both lines obtain marked core asymmetry from photospheric shocks in or near strong magnetic concentrations, less from higher-up internetwork shocks that produce similar asymmetry in the spatially averaged CaII 8542 profile.
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