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- W3012000980 abstract "The solar photospheric Fe abundance has been de- termined using realistic ab initio 3D, time-dependent, hydro- dynamical model atmospheres. The study is based on the ex- cellent agreement between the predicted and observed line pro- files directly rather than equivalent widths, since the intrinsic Doppler broadening from the convective motions and oscilla- tions provide the necessary non-thermal broadening. Thus, three of the four hotly debated parameters (equivalent widths, micro- turbulence and damping enhancement factors) in the center of the recent solar Fe abundance dispute regarding Fei lines no longer enter the analysis, leaving the transition probabilities as the main uncertainty. Both Fei (using the samples of lines of both the Oxford and Kiel studies) and Feii lines have been in- vestigated, which give consistent results: log FeI =7 :440:05 and log FeII =7 :45 0:10: Also the wings of strong Fei lines return consistent abundances, log FeII =7 :42 0:03; but due to the uncertainties inherent in analyses of strong lines we give this determination lower weight than the results from weak and intermediate strong lines. In view of the recent slight downward revision of the meteoritic Fe abundance log Fe =7 :46 0:01, the agreement between the meteoritic and photospheric values is very good, thus appearingly settling the debate over the pho- tospheric Fe abundance from Fei lines." @default.
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- W3012000980 date "2000-07-01" @default.
- W3012000980 modified "2023-09-26" @default.
- W3012000980 title "Line formation in solar granulation. II. The photospheric Fe abundance" @default.
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