Abstract:
The behavior of the line profiles in the wings of the first four lines of the Balmer, Paschen and Brackett series in the solar spectrum at the disc centre has been investigated with a view to comparing the computed profiles (Holweger & Muiler 1974; Vernazza, Avrett & Loeser 1976, 1981) with observations. The comparison shows that, in general, the HOlweger & Muller model can explain the lines of Balmer series better than the lines of Paschen and of Brackett series. The reverse is the case with the Vernazza, Avrett & Loeser Models.
