The MEGaN project I. Missing formation of massive nuclear clusters and
  tidal disruption events by star clusters - massive black hole interactions
  We investigated the evolution of a massive galactic nucleus hosting a
super-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 NSC
through GCs orbital decay and merger is efficiently inhibited by the tidal
forces exerted from the SMBH. The GCs mass loss induced by tidal forces causes
a significant modification of their mass function, leading to a population of
low-mass ($<10^4$) clusters. Nonetheless, the GCs debris accumulated around the
SMBH give rise to well-defined kinematical and morphological properties,
leading to the formation of a disk-like structure. Interestingly, the disk is
similar to the one observed in the M31 galaxy nucleus, which has properties
similar to our numerical model. The simulation produced a huge amount of data,
which we used to investigate whether the GC debris deposited around the SMBH
can enhance the rate of tidal disruption events (TDEs) in our galaxy inner
density distribution. Our results suggest that the GCs disruption shapes the
SMBH 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 of
galaxies with similar density profiles and central SMBHs. The simulation
presented here is the first of its kind, representing a massive galactic
nucleus and its star cluster population on scales $\sim 100$ pc.
