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Star-forming galaxies like the Milky Way are surrounded by a hot gaseous haloat the virial temperature - the so-called galactic corona - that plays afundamental role in their evolution. The interaction between the disc and thecorona has been shown to have a direct impact on accretion of coronal gas ontothe disc with major implications for galaxy evolution. In this work, we studythe gas circulation between the disc and the corona of star-forming galaxieslike the Milky Way. We use high-resolution hydrodynamical N-body simulations ofa Milky Way-like galaxy with the inclusion of an observationally-motivatedgalactic corona. In doing so, we use SMUGGLE, an explicit interstellar medium(ISM) and stellar feedback model coupled with the moving-mesh code Arepo. Wefind that the reservoir of gas in the galactic corona is sustaining starformation: the gas accreted from the corona is the primary fuel for theformation of new stars, helping in maintaining a nearly constant level of coldgas mass in the galactic disc. Stellar feedback generates a gas circulationbetween the disc and the corona (the so-called galactic fountain) by ejectingdifferent gas phases that are eventually re-accreted onto the disc. Theaccretion of coronal gas is promoted by its mixing with the galactic fountainsat the disc-corona interface, causing the formation of intermediate temperaturegas that enhance the cooling of the hot corona. We find that this process actsas a positive feedback mechanism, increasing the accretion rate of coronal gasonto the galaxy.

Galactic coronae in Milky Way-like galaxies: the role of stellar feedback in gas accretion