  The 16Cyg binary system hosts the solar-like Kepler targets with the most
stringent observational constraints. Moreover, this system is particularly
interesting since both stars are very similar in mass but the A component is
orbited by a red dwarf, whereas the B component is orbited by a Jovian planet
and thus could have formed a more complex planetary system. In our previous
study, we showed that seismic inversions of integrated quantities could be used
to constrain microscopic diffusion in the A component. In this study, we
analyse the B component in the light of a more regularised inversion. We wish
to analyse independently the B component of the 16Cyg binary system using the
inversion of an indicator dedicated to analyse core conditions, denoted tu.
Using this independent determination, we wish to analyse any differences
between both stars due to the potential influence of planetary formation on
stellar structure and/or their respective evolution. First, we recall the
observational constraints for 16CygB and the method we used to generate
reference stellar models. The inversion results were then used to analyse the
differences between the A and B components. The tu indicator for 16CygB shows a
disagreement with models including microscopic diffusion and sharing the
chemical composition previously derived for 16CygA. Small changes in chemical
composition are insufficient to solve the problem but that extra mixing can
account for the differences seen between both stars. We use a parametric
approach to analyse the impact of extra mixing in the form of turbulent
diffusion on the behaviour of the tu values. We conclude on the necessity of
further investigations using models with a physically motivated implementation
of extra mixing including additional constraints to further improve the
accuracy with which the fundamental parameters of this system are determined.
