All Tables

• Table 1: Visual and absolute magnitudes, B-V color, Hipparcos parallaxes, stellar masses (derived iterativey during the abundance analysis using the spectroscopic temperatures and abundances), and projected binary separation for program stars. The formal errors on magnitudes and colors are probably underestimated (see Paper I).
• Table 4: Adopted atmospheric parameters.
• Table 7: Results of differential analysis.
• Table 11: Final abundance difference (Fe I from Table 7) and estimates of the iron possibly accreted.
• Table 2: Magnitude difference for program stars.
• Table 5: Results of abundance analysis for primaries.
• Table 6: Temperature difference using different methods. The weighted average between the temperature difference based on the ionization equilibrium of iron and vanadium was adopted because of its higher accuracy.
• Table 8: Sensitivity to abundance and temperature difference when changing of atmospheric parameters for a few selected pairs.
• Table 9: Mean slopes of the variations in abundance difference and temperature difference between the components due to changes in the atmospheric parameters of the secondary.
• Table 10: Comparison of our analysis of HIP 76603/2 with that by Fuhrmann (2004).