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Following up our recent analysis devoted to the impact of non steadyaccretion on the location of young low-mass stars or brown dwarfs in theHerzsprung-Russell diagram, we perform a detailed analysis devoted to theeffect of burst accretion on the internal structure of low-mass and solar typestars. We find that episodic accretion can produce objects with significantlyhigher central temperatures than the ones of the non accreting counterparts ofsame mass and age. As a consequence, lithium depletion can be severely enhancedin these objects. This provides a natural explanation for the unexpected levelof lithium depletion observed in young objects for the inferred age of theirparent cluster. These results confirm the limited reliability of lithiumabundance as a criterion for assessing or rejecting cluster membership. Theyalso show that lithium is not a reliable age indicator, because its fatestrongly depends on the past accretion history of the star. Under theassumption that giant planets primarily form in massive disks prone togravitational instability and thus to accretion burst episodes, the sameanalysis also explains the higher Li depletion observed in planet hostingstars. At last, we show that, depending on the burst rate and intensity,accretion outbursts can produce solar mass stars with lower convective envelopemasses, at ages less than a few tens of Myr, than predicted by standard (non orslowly accreting) pre-main sequence models. This result has interesting,although speculative, implications for the recently discovered depletion ofrefractory elements in the Sun.

Effect of episodic accretion on the structure and the lithium depletion of low-mass stars and planet-hosting stars