Mn I 5394.7的活度灵敏度说明
Explanation of the activity sensitivity of Mn I 5394.7 Å
摘要：
关于太阳辐照度谱中Mn I 5394.7 A谱线在大活动时比大多数其他光球谱线更亮的原因，长期存在争议。这种活动敏感性是由Mg II h & k的色球发射光谱联锁引起的说法是有争议的。采用经典的一维建模方法进行论证，采用现代的三维磁流体模拟方法进行验证和分析。Mn I 5394.7 A谱线对太阳活动异常敏感，这要归功于它的超精细结构。这就克服了其他较窄的光球线失去这种灵敏度的热多普勒拖尾效应和颗粒多普勒拖尾效应。我们以邻近的Fe I 5395.2 A线为例，详细分析了这两条线的形成，以证明和解释颗粒多普勒增亮。我们表明，这会影响所有的窄线。无论是色球，也没有Mg II H & K发挥的作用，也是不正确的描述活动的灵敏度Mn I 5394.7 A通过plage模型与向外增加的温度对比。Mn I 5394.7 A线代表了太阳光球层深处强磁场浓度的代用诊断，与G波段和H-α的蓝翼相当，但不是比这些更好的。Mn I线在高分辨率Stokes偏振测量中作为弱场的诊断更有前途。
英文摘要：
There is a long-standing controversy concerning the reason why the Mn I 5394.7 A line in the solar irradiance spectrum brightens more at larger activity than most other photospheric lines. The claim that this activity sensitivity is caused by spectral interlocking to chromospheric emission in Mg II h & k is disputed. Classical one-dimensional modeling is used for demonstration; modern three-dimensional MHD simulation for verification and analysis. The Mn I 5394.7 A line thanks its unusual sensitivity to solar activity to its hyperfine structure. This overrides the thermal and granular Doppler smearing through which the other, narrower, photospheric lines lose such sensitivity. We take the nearby Fe I 5395.2 A line as example of the latter and analyze the formation of both lines in detail to demonstrate and explain granular Doppler brightening. We show that this affects all narrow lines. Neither the chromosphere nor Mg II h & k play a role, nor is it correct to describe the activity sensitivity of Mn I 5394.7 A through plage models with outward increasing temperature contrast. The Mn I 5394.7 A line represents a proxy diagnostic of strong-field magnetic concentrations in the deep solar photosphere comparable to the G band and the blue wing of H-alpha, but not a better one than these. The Mn I lines are more promising as diagnostic of weak fields in high-resolution Stokes polarimetry.
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