N-body simulation of two-dimensional stationary stellar distributions: Dissipation of energy and development of the field of velocity
- 33 Downloads
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.
KeywordsConstant Time Central Region Velocity Field Velocity Vector Massive Particle
Unable to display preview. Download preview PDF.
- Brigham, E. O.: 1974,The Fast Fourier Transform, pp. 148 and 198.Google Scholar
- Hohl, F.: 1970,Dynamical Evolution of Disk Galaxy, NASA Tr R-343.Google Scholar
- Hohl, F. and Hockney, R. W.: 1969,J. Computational Phys. 4, 306.Google Scholar
- Liu Bulin: 1984,Chin. Astron. Astrophys. 8, 310.Google Scholar
- Miller, R. H.: 1976,J. Computational Phys. 21, 400–437.Google Scholar
- Thielheim, K. O. and Wolff, H.: 1984,Astrophys. J. 276, 135.Google Scholar
- Thielheim, K. O. and Wolff, H.: 1985, in H. van Woerden, R. J. Allen, and W. B. Burton (eds.), ‘The Milky Way Galaxy’,IAU Symp. 106, 539.Google Scholar