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I present examples of how chemo-dynamical N-body simulations can helpunderstanding the structure and evolution of the inner Galaxy. Such simulationsreproduce the observed links between kinematics, morphology and chemistry inthe bar/bulge region and explain them by the self-consistent cohabitation of anumber of components. Galactic archaeology, applied to simulation snapshots,explains the sequence in which the stars of the various components were formed.The thick disc stars form earlier than those of the thin disc and in a muchshorter time scale. The bar in the thick disc is horizontally thicker than thatof the thin disc and has a different vertical morphology. The Galaxy's innerdisc scalelength is much smaller than what is expected from nearby galaxies ofsimilar stellar mass.

Using N-body simulations to understand the chemo-dynamical evolution of the inner Milky Way