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Aims: We study the effects of the cosmological assembly history on thechemical and dynamical properties of the discs of spiral galaxies as a functionof radius. Methods: We make use of the simulated Milky-Way mass,fully-cosmological discs, from {\tt RaDES} (Ramses Disc Environment Study). Weanalyse their assembly history by examining the proximity of satellites to thegalactic disc, instead of their merger trees, to better gauge which satellitesimpact the disc. We present stellar age and metallicity profiles,Age-Metallicity Relation (AMR), Age-Velocity dispersion Relation (AVR), andStellar Age Distribution (SAD) in several radial bins for the simulatedgalaxies. Results: Assembly histories can be divided into three differentstages: i) a merger dominated phase, when a large number of mergers with massratios of $\sim$1:1 take place (lasting $\sim$3.2$\pm$0.4 Gyr on average); ii)a quieter phase, when $\sim$1:10 mergers take place (lasting $\sim$4.4$\pm$2.0Gyr) - these two phases are able to kinematically heat the disc and produce adisc that is chemically mixed over its entire radial extension; iii) a"secular" phase where the few mergers that take place have mass ratios below1:100, and which do not affect the disc properties (lasting $\sim$5.5$\pm$2.0Gyr). Phase ii ends with a final merger event (at time $t_\mathrm{jump}$)marking the onset of important radial differences in the AMR, AVR, and SAD.Conclusions: Inverted AMR trends in the outer parts of discs, for stars youngerthan $t_\mathrm{jump}$, are found as the combined effect of radial motions andstar formation in satellites temporarily located in these outer parts."U-shaped" stellar age profiles change to an old plateau ($\sim$10 Gyr) in theouter discs for the entire {\tt RaDES} sample. This shape is a consequence ofinside-out growth of the disc, radial motions of disc stars ... [abridged]

The imprint of satellite accretion on the chemical and dynamical properties of disc galaxies