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

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4. Line computations

Most of spectral line computations were performed with the code SPANSAT (Gadun & Sheminova 1988) in LTE. Equivalent width computations for Li I lines were carried out with the program WITA2 (Pavlenko et al. 1995). Van der Waals broadening with the correction factor [FORMULA] and Stark broadening were taken into account. It is interesting to note that the central intensities of spectral lines are more sensitive to NLTE effects (see GK89) than equivalent widths. For this reason, to study the impact of photospheric inhomogeneities on Li and Fe abundances we analise [FORMULA] only.

4.1. 1-D, OGA, and MSA models

The motion field was treated in the frame of a height-independent microturbulent velocity ([FORMULA]). All computations with 1-D models were performed with [FORMULA] = 1 km/s. To fit the central intensity of the Li I line we also used a height-independent macroturbulent velocity [FORMULA] = 1.85 km/s.

4.2. 2D models

Absorption lines of iron and lithium were computed for every vertical column of the model region. Afterwards the line profiles were averaged over space and modeling time as in Paper I.

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© European Southern Observatory (ESO) 1997

Online publication: May 26, 1998

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