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We investigated the evolution of a massive galactic nucleus hosting asuper-massive black hole (SMBH) with mass $M_\mathrm{SMBH}=10^8\mathrm{M}_\odot$ surrounded by a population of 42 heavy star clusters (GCs).Using direct $N$-body modelling, we show here that the assembly of an NSCthrough GCs orbital decay and merger is efficiently inhibited by the tidalforces exerted from the SMBH. The GCs mass loss induced by tidal forces causesa significant modification of their mass function, leading to a population oflow-mass ($<10^4$) clusters. Nonetheless, the GCs debris accumulated around theSMBH give rise to well-defined kinematical and morphological properties,leading to the formation of a disk-like structure. Interestingly, the disk issimilar to the one observed in the M31 galaxy nucleus, which has propertiessimilar to our numerical model. The simulation produced a huge amount of data,which we used to investigate whether the GC debris deposited around the SMBHcan enhance the rate of tidal disruption events (TDEs) in our galaxy innerdensity distribution. Our results suggest that the GCs disruption shapes theSMBH neighbourhoods leading to a TDE rate of $\sim 2 \times 10^{-4} $yr$^{-1}$,a value slightly larger than what expected in previous theoretical modelling ofgalaxies with similar density profiles and central SMBHs. The simulationpresented here is the first of its kind, representing a massive galacticnucleus and its star cluster population on scales $\sim 100$ pc.

The MEGaN project I. Missing formation of massive nuclear clusters and tidal disruption events by star clusters - massive black hole interactions