... binaries

Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.

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...

The equivalent widths are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/420/683

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... mixing

Alternative explanations of Li-dip depletion such as mass loss or gravitational sedimentation do not seem to be supported by observations, see Do Nascimento et al. (2000).

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... estimate

The comparison between the results quoted in the original papers show some inconsistencies because of different assumptions on the composition of meteoritic material. In this paper, we adopt the meteoritic abundances by Lodders (2003). The mass fraction of iron is thus 18.3% of the meteoritic material.

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... IRAF

IRAF is distributed by the National Optical Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Fundation.

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... details)

The equivalent widths are only available in electronic form at the CDS.

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... metallicity

The periods of the observed systems are too long for any reliable determination of dynamical masses (see Desidera et al. 2003 for the case of HD 219542).

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...$\pm$0.04 dex)

In the case of HD 132844A the procedure used for the other stars gives very high gravities ( $\log g=4.74$), This is likely due to a large error in parallaxes. For this star only, the analysis of the primary was purely spectroscopic, with the temperature derived from the excitation equilibrium and gravity from the ionization equilibrium.

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... region

As noted in Sect. 1, the extra-mixing mechanism producing the Li dip has some dependence on stellar age. This is not taken into account in our estimate of the mass of the mixing zone.

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... differences

Considering the observed planet frequency, and the differences of the mass of the convective zone between the components, it appears very unlikely that both components of a binary system have accreted such metal rich material that their original composition is alterated by a similar amount.

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