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

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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 [FORMULA] 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 [FORMULA] and [FORMULA] behaviour, where abundances [FORMULA] and [FORMULA] 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 [FORMULA] and [FORMULA] 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 [FORMULA] and [FORMULA] 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 [FORMULA] and [FORMULA] 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

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© European Southern Observatory (ESO) 1997

Online publication: May 26, 1998