We study the influence of rotation on the dynamical evolution of collisional single-mass stellar clusters up to core-collapse by using N-body simulations. Rotating King models which are characterized by dimensionless central potential parameter Wo and the rotation parameter Wo are used as initial models. Our results show that inner shells slowly contract until core-collapse phase is reached, followed by a slow expansion. Angular momentum is transported outward, while the core is rotating even faster than before, as predicted by gravogyro catastrophe theory. We confirm that rotation plays an important role in accelerating the dynamical evolution of stellar cluster, in particular in accelerating the core collapse.

• ELIANI ARDI(Yukawa Institute for Theoretical Physics, Kyoto University)
• RAINER SPURZEM(Astronomisches Rechen-Institute, Heidelberg)
• SHIN MINESHIGE(Astronomisches Rechen-Institute, Heidelberg)