  We discuss the structural change and degree of mass segregation of young
dense star clusters within about 100pc of the Galactic center. In our
calculations, which are performed with GRAPE-6, the equations of motion of all
stars and binaries are calculated accurately but the external potential of the
Galaxy is solved (semi)analytically. The simulations are preformed to model the
Arches star cluster. We find that star clusters with are less strongly
perturbed by the tidal field and dynamical friction are much stronger affected
by mass segregation; resulting in a significant pile-up of massive stars in the
cluster center. At an age of about 3.5Myr more than 90 per cent of the stars
more massive than ~10Msun are concentrated within the half-mass radius of the
surviving cluster. Star clusters which are strongly perturbed by the tidal
field of the parent Galaxy are much less affected by mass segregation.
