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Supermassive black holes at the centre of galactic nuclei mostly grow in massthrough gas accretion over cosmic time. This process also modifies the angularmomentum (or spin) of black holes, both in magnitude and in orientation.Despite being often neglected in galaxy formation simulations, spin plays acrucial role in modulating accretion power, driving jet feedback, anddetermining recoil velocity of coalescing black hole binaries. We present a newaccretion model for the moving-mesh code {\sc arepo} that incorporates (i) massaccretion through a thin $\alpha$-disc, and (ii) spin evolution through theBardeen-Petterson effect. We use a diverse suite of idealised simulations toexplore the physical connection between spin evolution and larger scaleenvironment. We find that black holes with mass $\lesssim 10^{7}$ M$_{\odot}$experience quick alignment with the accretion disc. This favours prolongedphases of spin-up, and the spin direction evolves according to the gas inflowon timescales as short as $\lesssim 100$ Myr, which might explain the observedjet direction distribution in Seyfert galaxies. Heavier black holes ($\gtrsim10^{8}$ M$_{\odot}$) are instead more sensitive to the local gas kinematic.Here we find a wider distribution in spin magnitudes: spin-ups are favoured ifgas inflow maintains a preferential direction, and spin-downs occur for nearlyisotropic infall, while the spin direction does not change much over shorttimescales $\sim 100$ Myr. We therefore conclude that supermassive black holeswith masses $\gtrsim 5 \times 10^{8}$ M$_{\odot}$ may be the ideal testbed todetermine the main mode of black hole fuelling over cosmic time.

Galactic nuclei evolution with spinning black holes: method and implementation