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We study the oxygen abundance profiles of the gas-phase components inhydrodynamical simulations of pre-prepared disc galaxies including majormergers, close encounters and isolated configurations. We analyse the evolutionof the slope of oxygen abundance profiles and the specific star formation rate(sSFR) along their evolution. We find that galaxy-galaxy interactions couldgenerate either positive and negative gas-phase oxygen profiles depending onthe state of evolution. Along the interaction, galaxies are found to havemetallicity gradients and sSFR consistent with observations, on average. Stronggas inflows produced during galaxy-galaxy interactions or as a result of stronglocal instabilities in gas-rich discs are able to produce both a quick dilutionof the central gas-phase metallicity and a sudden increase of the sSFR. Oursimulations show that, during these events, a correlation between themetallicity gradients and the sSFR can be set up if strong gas inflows aretriggered in the central regions in short timescales. Simulated galaxieswithout experiencing strong disturbances evolve smoothly without modifying themetallicity gradients. Gas-rich systems show large dispersion along thecorrelation. The dispersion in the observed relation could be interpreted asproduced by the combination of galaxies with different gas-richness and/orexperiencing different types of interactions. Hence, our findings suggest thatthe observed relation might be the smoking gun of galaxies forming in ahierarchical clustering scenario.

The evolution of the metallicity gradient and the star formation efficiency in disc galaxies