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N-body simulation of two-dimensional stationary stellar distributions: Dissipation of energy and development of the field of velocity

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Abstract

The procedure for the simulation of two-dimensionalN-body configurations described in this paper has been devised to investigate the dissipation of energy and the development of velocity in given sub-regions of stellar systems, especially in the central region of a galaxy. In these simulations massive particles are injected into the given spatial region at a pre-determined constant time rate and at a given distribution of velocity vectors. The mass points are allowed to interact gravitationally and special attention is given to the influence of near-by encounters. After a certain period of time a stationary (equilibrium) situation settles down with a certain distribution of mass points in position and velocity space. Preliminary results obtained so far demonstrate the reliability of this procedure forN-body simulation and for the investigation of the dissipation of energy and of the development of velocity fields. Forthcoming results are hoped to deliver information on the role of three-body encounters in the processes of randomization at work in self-consistent stellar configurations.

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J. Polcher and W. Wanner also of the Mathematical Physics Group of the IFK took part in many of the discussions concerning the development of this programme.

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Thielheim, K.O., Bulin, L. N-body simulation of two-dimensional stationary stellar distributions: Dissipation of energy and development of the field of velocity. Astrophys Space Sci 181, 43–53 (1991). https://doi.org/10.1007/BF00644111

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Keywords

  • Constant Time
  • Central Region
  • Velocity Field
  • Velocity Vector
  • Massive Particle