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Aims: The effects of rotation and magnetic fields on the surface abundancesof solar-type stars are studied in order to investigate whether the reporteddifference in lithium content of exoplanet-host stars can be related to theirrotational history. Moreover, the asteroseismic properties predicted for starswith and without exoplanets are compared to determine how such a scenario,which relates the lithium abundances and the rotational history of the star,can be further challenged by observations of solar-like oscillations. Methods:Based on observations of rotational periods of solar-type stars, slow rotatorson the zero age main sequence (ZAMS) are modelled with a comprehensivetreatment of only the shellular rotation, while fast rotators are modelledincluding both shellular rotation and magnetic fields. Assuming a possible linkbetween low rotation rates on the ZAMS and the presence of planets as a resultof a longer disc-locking phase during the pre-main sequence (PMS), we comparethe surface abundances and asteroseismic properties of slow and fast rotatingmodels, which correspond to exoplanet-host stars and stars without detectedplanets, respectively. Results: We confirm previous suggestions that thedifference in the lithium content of stars with and without detected planetscan be related to their different rotational history. The larger efficiency ofrotational mixing predicted in exoplanet-host stars explains their lithiumdepletion and also leads to changes in the structure and chemical compositionof the central stellar layers. Asteroseismic observations can reveal thesechanges and can help us distinguish between different possible explanations forthe lower lithium content of exoplanet-host stars.

Effects of rotation and magnetic fields on the lithium abundance and asteroseismic properties of exoplanet-host stars