Lithium and mass loss in massive AGB stars in the LargeMagellanic

The aim of this work is to use full evolutionary models to derive observational constraints on the mass loss rate of the upper Asymptotic Giant Branch (AGB) stars. The observations used to constrain the models are: i) the relative number of luminous Lithium rich AGBs in the Magellanic Clouds, with respect to the total number of AGBs populating the luminosity range ?6 M bol ?7; ii) the s{process enhancement of the same sample. The calibration of the mass loss rate we obtain gives feedbacks on the interpretation of observational data of obscured AGBs, and allows us to provide consistent lithium yields for these stars, to be used to constrain the galactic chemical evolution. We nd that: a) we can put lower and upper limits to the mass loss rate during the AGB phase; b) after a \visi-ble" phase, the models evolve into a phase of strong mass loss, which can be identiied with the obscured OH/IR stars accessible only in the infrared; the models well reproduce the Period{M bol loci of the obscured AGBs (Wood et al. 1992); c) the most massive AGBs (mass of progenitors , hereinafter M ZAMS , 6M) are extremely luminous (M bol ?7:2 to ?7:5); d) The lithium yield increases with the mass loss rate and with the total stellar mass, being maximum for AGB stars close to the lower limit for carbon semi-degenerate ignition. However, the mass loss calibration obtained in this work implies that massive AGBs do not contribute signiicantly to the lithium enrichment of the interstellar medium.