  In the standard model of structure formation, galaxies form in the centre of
dark matter haloes that develop as a result of inhomogeneities in the
primordial mass distribution of the Universe. Afterwards, galaxies grow by
means of continuous accretion of gaseous material stemming from the
intergalactic medium, both in diffuse form and through collisions with other
systems. After an initial period of violent growth, the gas settles into a
rotationally-supported structure where stars are born, giving birth to the
stellar disc. The accretion of gaseous material onto the disc plays a
fundamental role in its evolution as it can change its dynamical and
morphological properties, generating gas flows within the disc. In this work,
we use 30 galaxies from the Auriga Project, a set of cosmological
magnetohydrodynamical simulations of disc galaxies, to study the temporal
dependence of the gas accretion rates, focusing on the inflowing and outflowing
fluxes.
