  In this paper we report results of collisional N-body simulations of the
dynamical evolution of equal-mass star clusters containing a massive central
black hole. Each cluster is composed of between 5,000 to 180,000 stars together
with a central black hole which contains between 0.2% to 10% of the total
cluster mass.
  We find that for large enough black hole masses, the central density follows
a power-law distribution with slope \rho \sim r^{-1.75} inside the radius of
influence of the black hole, in agreement with predictions from earlier Fokker
Planck and Monte Carlo models. The tidal disruption rate of stars is within a
factor of two of that derived in previous studies. It seems impossible to grow
an intermediate-mass black hole (IMBH) from a M \le 100 Msun progenitor in a
globular cluster by the tidal disruption of stars, although M = 10^3 Msun IMBHs
can double their mass within a Hubble time in dense globular clusters. The same
is true for the supermassive black hole at the centre of the Milky Way.
  Black holes in star clusters will feed mainly on stars tightly bound to them
and the re-population of these stars causes the clusters to expand, reversing
core-collapse without the need for dynamically active binaries. Close
encounters of stars in the central cusp also lead to an increased mass loss
rate in the form of high-velocity stars escaping from the cluster. A companion
paper will extend these results to the multi-mass case.
