The imprint of satellite accretion on the chemical and dynamical
  properties of disc galaxies
  Aims: We study the effects of the cosmological assembly history on the
chemical and dynamical properties of the discs of spiral galaxies as a function
of radius. Methods: We make use of the simulated Milky-Way mass,
fully-cosmological discs, from {\tt RaDES} (Ramses Disc Environment Study). We
analyse their assembly history by examining the proximity of satellites to the
galactic disc, instead of their merger trees, to better gauge which satellites
impact the disc. We present stellar age and metallicity profiles,
Age-Metallicity Relation (AMR), Age-Velocity dispersion Relation (AVR), and
Stellar Age Distribution (SAD) in several radial bins for the simulated
galaxies. Results: Assembly histories can be divided into three different
stages: i) a merger dominated phase, when a large number of mergers with mass
ratios 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$2.0
Gyr) - these two phases are able to kinematically heat the disc and produce a
disc that is chemically mixed over its entire radial extension; iii) a
"secular" phase where the few mergers that take place have mass ratios below
1:100, and which do not affect the disc properties (lasting $\sim$5.5$\pm$2.0
Gyr). 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 younger
than $t_\mathrm{jump}$, are found as the combined effect of radial motions and
star formation in satellites temporarily located in these outer parts.
"U-shaped" stellar age profiles change to an old plateau ($\sim$10 Gyr) in the
outer discs for the entire {\tt RaDES} sample. This shape is a consequence of
inside-out growth of the disc, radial motions of disc stars ... [abridged]
