  Li-depleted (enhanced) stars in the main-sequence (MS) and (or) the RGB, pose
a puzzling mystery. Presently, there is still no clear answer to the
mechanism(s) that enables such Li depletion (enhancement). One possible
explanation comes from the, still controversial, observational evidence of Li
underabundances in MS stars hosting planets, and of a positive correlation
between the Li abundance and rotational velocity in some RGB stars, which
suggests a stellar collision with a planet-like object as a possible solution.
In this study we explore this scenario, performing for first time
3D-hydrodynamical simulations of a 0.019 Mo brown dwarf collision with a MS
star under different initial conditions. This enables us to gather information
about the impact on the physical structure and final Li content in the hosting
star.
