We have derived beryllium abundances in a wide sample of stars hosting planets , with spectral types in the range F7V - K0V , aimed at studying in detail the effects of the presence of planets on the structure and evolution of the associated stars .
Predictions from current models are compared with the derived abundances and suggestions are provided to explain the observed inconsistencies .
We show that while still not clear , the results suggest that theoretical models may have to be revised for stars with T _ { \mathrm { eff } } < 5500 K. On the other hand , a comparison between planet host and non-planet host stars shows no clear difference between both populations .
Although preliminary , this result favors a “ primordial ” origin for the metallicity “ excess ” observed for the planetary host stars .
Under this assumption , i.e .
that there would be no differences between stars with and without giant planets , the light element depletion pattern of our sample of stars may also be used to further investigate and constraint Li and Be depletion mechanisms .