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While the metallicity excess observed in the central stars of planetary systems is confirmed by all recent observations, the reason for this excess is still a subject of debate : is it primordial, is it the result of accretion or both? The basic argument against an accretion origin is related to the masses of the outer convective zones which vary by more than one order of magnitude among the considered stars while the observed overabundances of metals are similar. We show here that in previousdoi:10.1086/382668 fatcat:67xdfvkoazadbk6bolgy56galm