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In the standard paradigm of galaxy formation and evolution, the baryoniccomponent of galaxies forms from the collapse and condensation of gas withindark matter haloes, and later grows from continuous accretion of gaseous mass,both in diffuse form and in mergers with other systems. After a first period ofrapid and violent halo growth, the gas settles into a rotationally-supportedstructure, eventually giving rise to the formation of a stellar disc. Starsevolve and return chemically-processed gas and energy to the interstellarmedium, mainly through Type II supernova explosions. In the disc region, thecosmological accretion of gas combines with the outflows resulting fromsupernovae, affecting the hydrodynamical and structural properties of the discand producing gas flows in the vertical and radial directions. In this work, weuse a simulation of the Auriga Project, a suite of magneto-hydrodynamical,zoom-in cosmological simulations of Milky Way-like galaxies, to study thetemporal and radial dependencies of gas accretion onto the disc. We alsoinvestigate the disc evolution, focusing on the inside-out disc formationscenario, which is one of the fundamental hypotheses of chemical evolutionmodels of the Galaxy.

Gas accretion onto the disc of a simulated Milky Way-mass galaxy