论文标题
磁化太阳大气中光谱线的诊断：黑子中H \ b {eta}线的形成
Diagnostic of Spectral Lines in Magnetized Solar Atmosphere: Formation of the H\b{eta} Line in Sunspots
论文作者
论文摘要
H $β$ $ $λ$4861.34Å线的形成是与诊断太阳能和恒星色球中磁场的基本配置有关的重要主题。具体而言，由于太阳能大气中的磁性和微电场，宽阔的h $β$β$ $ $ $λ$4861.34Å。基于非本地热力学平衡的假设，提出了模型中H $β$的形成。 It is found that the model umbral chromosphere is transparent to the Stokes parameters of the H$β$ line, which implies that the observed signals of magnetic fields at sunspot umbrae via the H$β$ line originate from the deep solar atmosphere, where $\lg τ_c\approx-1$ (about 300 km in the photospheric layer for our calculations).这与观察到的stokes信号相反，该信号来自非阳离子区域，这些信号被认为主要是在太阳能球体中形成的。
Formation of the H$β$ $λ$4861.34 Å line is an important topic related to the diagnosis of the basic configuration of magnetic fields in the solar and stellar chromospheres. Specifically, broadening of the H$β$ $λ$4861.34 Å line occurs due to the magnetic and micro-electric fields in the solar atmosphere. The formation of H$β$ 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 H$β$ line, which implies that the observed signals of magnetic fields at sunspot umbrae via the H$β$ line originate from the deep solar atmosphere, where $\lg τ_c\approx-1$ (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.
