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. As discussed in the text, the formal errors
on magnitudes and colors are likely underestimated.
- Table 2:
Magnitude difference for program stars.
- Table 3:
Adopted atmospheric parameters.
- Table 4:
Results of abundance analysis for primaries.
- Table 5:
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 6:
Sensitivity to abundance and temperature difference to changes
of atmospheric parameters for the pair HD 219542.
- Table 7:
Results of differential analysis.
- Table 8:
Final abundance difference (Fe I from Table 7)
and estimates of iron possibly accreted.