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We analyse the output of the hi-res cosmological zoom-in simulation ErisBH tostudy self-consistently the formation of a strong stellar bar in a MilkyWay-type galaxy and its effect on the galactic structure, on the central gasdistribution and on star formation. The simulation includes radiative cooling,star formation, SN feedback and a central massive black hole which isundergoing gas accretion and is heating the surroundings via thermal AGNfeedback. A large central region in the ErisBH disk becomes bar-unstable afterz~1.4, but a clear bar-like structure starts to grow significantly only afterz~0.4, possibly triggered by the interaction with a massive satellite. At z~0.1the bar reaches its maximum radial extent of l~2.2 kpc. As the bar grows, itbecomes prone to buckling instability, which we quantify based on theanisotropy of the stellar velocity dispersion. The actual buckling event isobservable at z~0.1, resulting in the formation of a boxy-peanut bulge clearlydiscernible in the edge-on view of the galaxy at z=0. The bar in ErisBH doesnot dissolve during the formation of the bulge but remains stronglynon-axisymmetric down to the resolution limit of ~100 pc at z=0. During itsearly growth, the bar exerts a strong torque on the gas within its extent anddrives gas inflows that enhance the nuclear star formation on sub-kpc scales.Later on the infalling gas is nearly all consumed into stars and, to a lesserextent, accreted onto the central black hole, leaving behind a gas-depletedregion within the central ~2 kpc. Observations would more likely identify aprominent, large-scale bar at the stage when the galactic central region hasalready been quenched. Bar-driven quenching may play an important role indisk-dominated galaxies at all redshift. [Abridged]

Bar-driven evolution and quenching of spiral galaxies in cosmological simulations