Formation of the Hβ λ4861.34 Å line is an important topic related to the diagnosis of the basic configuration of magnetic fields in the solar and stellar chromospheres. Specifically, broadening of the Hβ λ4861.34 Å line occurs due to the magnetic and micro-electric fields in the solar atmosphere. The formation of Hβ in the model umbral atmosphere is presented based on the assumption of non-local thermodynamic equilibrium. It is found that the model umbral chromosphere is transparent to the Stokes parameters of the Hβ line, which implies that the observed signals of magnetic fields at sunspot umbrae via the Hβ line originate from the deep solar atmosphere, where lg τ_c ≈ −1 (about 300 km in the photospheric layer for our calculations). This is in contrast to the observed Stokes signals from non-sunspot areas, which are thought to primarily form in the solar chromosphere.

中文翻译：

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磁化太阳大气中光谱线的诊断：黑子中Hβ线的形成

的H形成βλ 4861.34的线是与在太阳能和恒星色球磁场的基本配置的诊断的一个重要课题。具体地，H的扩大β λ 4861.34的线的发生是由于在太阳能气氛中的磁性和微电场。H的形成β在模型哑气氛是基于非本地热力学平衡的假设呈现。据发现，该模型哑色球是透明的H的斯托克斯参数β线，这意味着在太阳黑子umbrae经由为H磁场的观测信号β线从深太阳大气，其中LGτ起源_Ç≈-1（在我们的计算中，在光球层中约为300 km）。这与从非黑子区域观察到的斯托克斯信号相反，后者被认为主要形成于太阳色球层。