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The early evolution of planetary systems is expected to depend on variousperiods of disk matter accretion onto the central star, which may include theaccretion of metal-rich matter after the star settles on the main sequence.When this happens, the accreted material is rapidly mixed within the surfaceconvective zone and induces an inverse mean-molecular-weight gradient, unstablefor thermohaline convection. The induced mixing, which dilutes the metalexcess, may also have important consequences on the light elements abundances.We model and analyze this process, and present the results according to variouspossible accretion scenarios. We give a detailed discussion of the differentways of treating thermohaline mixing, as proposed by previous authors, and weconverge on a consistent view, including the most recent numerical simulations.We show how the observations of light elements in stars can be used as tracersof such events.

Metal-rich accretion and thermohaline instabilities in exoplanets-host stars: consequences on the light elements abundances