摘要
Formation of the Hβλ4861.34Aline 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 Hβλ4861.34Aline occurs due to the magnetic and microelectric fields in the solar atmosphere.The formation of Hβin 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 Hβline,which implies that the observed signals of magnetic fields at sunspot umbrae via the Hβline originate from the deep solar atmosphere,where lgτc≈-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.
基金
supported by the National Natural Science Foundation of China(Grant Nos.11673033,11427803,and 11427901)。
