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Recent studies have argued that galaxy mergers are not important drivers forthe evolution of S0's, on the basis that mergers cannot preserve the couplingbetween the bulge and disk scale-lengths observed in these galaxies and thelack of correlation of their ratio with the S0 Hubble type. We investigatewhether the remnants resulting from collision-less N-body simulations ofintermediate and minor mergers onto S0 galaxies evolve fulfilling globalstructural relations observed between the bulges and disks of these galaxies.Different initial bulge-to-disk ratios of the primary S0 have been considered,as well as different satellite densities, mass ratios, and orbits of theencounter. We have analysed the final morphology of the remnants in imagessimulating the typical observing conditions of S0 surveys. We derive bulge+diskdecompositions of the final remnants to compare their global bulge-to-diskstructure with observations. We show that all remnants present undisturbed S0morphologies according to the prescriptions of specialized surveys. The dryintermediate and minor mergers induce noticeable bulge growth (S0c --> S0b andS0b --> S0a), but affect negligibly to the bulge and disk scale-lengths.Therefore, if a coupling between these two components exists prior to themerger, the encounter does not break this coupling. This fact provides a simpleexplanation for the lack of correlation between the ratio of bulge and diskscale-lengths and the S0 Hubble type reported by observations. These modelsprove that dry intermediate and minor mergers can induce global structuralevolution within the sequence of S0 Hubble types compatible with observations,meaning that these processes should not be discarded from the evolutionaryscenarios of S0's just on the basis of the strong coupling observed between thebulge and disk scale-lengths in these galaxies (abridged).

Evolution along the sequence of S0 Hubble types induced by dry minor mergers. I - Global bulge-to-disk structural relations