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We have used high-resolution spectra obtained with the multifiber facilityFLAMES at the Very Large Telescope of the European Southern Observatory toderive kinematic properties and chemical abundances of Fe, O, Mg and Si for 89stars in the disk of the Large Magellanic Cloud (LMC). The derived metallicityand [alpha/Fe], obtained as the average of O, Mg and Si abundances, allow us todraw a preliminary scheme of the star formation history occurred in this regionof the LMC. The derived metallicity distribution shows two main components: onecomponent (comprising ~ 84% of the sample) is peaked at [Fe/H] = -0.48 dex andit shows an [alpha/Fe] ratio slightly under solar ([alpha/Fe] ~ -0.1 dex). Thispopulation was probably originated by the main star formation event occurred3-4 Gyr ago (possibly triggered by tidal capture of the Small MagellanicCloud). The other component (comprising ~ 16% of the sample) is peaked at[Fe/H] ~ -1 dex and it shows an [alpha/Fe] ~ 0.2 dex. This population wasprobably generated during the long quiescent epoch of star formation in betweenthe first episode and the most recent bursts. Indeed, in our sample we do notfind stars with chemical properties similar to the old LMC globular clustersnor to the iron-rich and alpha-poor stars recently found in the LMC globularcluster NGC 1718 and predicted to be also in the LMC field, thus suggestingthat both these components are small (< 1%) in the LMC disk population.

Tagging the Chemical Evolution History of the Large Magellanic Cloud Disk