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DYNAMICAL EVOLUTION OF ROTATING SINGLE-MASS STELLAR CLUSTER

  • ARDI ELIANI (Yukawa Institute for Theoretical Physics, Kyoto University) ;
  • SPURZEM RAINER (Astronomisches Rechen-Institute, Heidelberg) ;
  • MINESHIGE SHIN (Astronomisches Rechen-Institute, Heidelberg)
  • Published : 2005.06.01

Abstract

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 $W_o$ and the rotation parameter $W_o$ 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.

Keywords

stellar dynamics;methods: n-body simulations

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  2. N-body models of rotating globular clusters vol.377, pp.2, 2007, https://doi.org/10.1111/j.1365-2966.2007.11602.x
  3. 2D Fokker-Planck models of rotating clusters vol.373, pp.2, 2006, https://doi.org/10.1111/j.1365-2966.2006.11036.x
  4. Higher-order moment models of dense stellar systems: applications to the modelling of the stellar velocity distribution function vol.410, pp.1, 2011, https://doi.org/10.1111/j.1365-2966.2010.17454.x