We discuss the structural change and degree of mass segregation of young dense star clusters within about 100 pc 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 3.5 Myr more than 90 per cent of the stars more massive than \sim 10 { M } _ { \odot } 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 .