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Astron. Astrophys. 342, 610-613 (1999)

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4. Solar iron abundance

In Table 2 our log(gf) values, equivalent widths and iron abundance data are listed. The log(gf) values are taken from Heise & Kock (1990) but rescaled with our new lifetime data. The reference lines marked with a are also rescaled. Following our former model-atmosphere analysis our new abundance values become slightly lower than in Holweger et al. (1990), because of the enlarged log(gf) values. The final solar iron abundance resulting from the entire sample of Fe II lines becomes

[EQUATION]

on the usual scale with log N(H)=12. Following Holweger et al. (1990) the three infrared lines marked with b are half weighted. The quoted uncertainty refer to the internal accuracy, i.e. the standard deviation of the individual lines. This corresponds to a standard deviation of the mean of less than 0.05 dex which is also quoted in Hannaford et al. (1992). The difference to their result of 7.48 [FORMULA] 0.04 is a consequence of different f-values (-0.007 dex), equivalent widths (-0.005 dex), Van-der-Waals-broadening (-0.017 dex) and a different weighting of the individual lines.


[TABLE]

Table 2. Solar iron abundance


As shown in Figs. 4, 5 and 6 no significant dependence of abundance on equivalent width, log(gf) value and wavelength exists, with the possible exception of the three infrared lines (shown as thin crosses). It is a remarkable outcome of the present paper that the solar iron abundance has shifted to a still lower value compared to that of Blackwell et al. (1984).

[FIGURE] Fig. 4. Solar iron abundance versus equivalent width

[FIGURE] Fig. 5. Solar iron abundance versus log(gf) value

[FIGURE] Fig. 6. Solar iron abundance versus wavelength

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© European Southern Observatory (ESO) 1999

Online publication: February 22, 1999
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