Astron. Astrophys. 324, 281-288 (1997)

3. Line lists

The lists of weak Fe I and Fe II lines used are given in Tables 1 and 2, respectively. They were taken for a comparative analysis of iron abundance determination based on the chosen sets of 1-D and 2-D models. Central depths and equivalent widths of these lines observed in the solar spectrum were taken from Gurtovenko & Kostyk (1989: GK89). Note, the weak Fe I and Fe II lines were selected from Paper I, and were used there to obtain the iron abundance based on earlier 3-D models. Our Fe I lines have laboratory determined oscillator strengths by Blackwell et al. (1979, 1986). For the set of FeII lines we took the empirical oscillator strengths of Gurtovenko & Kostyk (1989) which are consistent with the Oxford system of oscillator strengths. For the Li I resonance doublet at 670.8 nm, we used data from Wiese et al. (1966).

To investigate how the 2-D HD models reproduce the profiles of spectral lines forming at different levels of the solar atmosphere, we analyzed the and behaviour, where abundances and were determined by the fit of equivalent widths and central intensities of absorption lines in the center of the Sun, respectively ¹. For this, we added a sample of stronger lines into Table 1 and Table 2. So, for OG models we used the whole list from Paper I containing 42 Fe I and 32 Fe II lines and for MS models and computations were performed for 17 Fe I and 18 Fe II lines only. In last case we used reduced set of lines from Paper I because and for MS models vary in dependence on line parameters not so strong as in the case of OG models. Preliminary results concerning the relative behavior of and of Fe I and Fe II lines for these 2-D models have been represented by Gadun (1996).

Table 1. List of Fe I lines

Table 2. List of Fe II lines

© European Southern Observatory (ESO) 1997

Online publication: May 26, 1998

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