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N-Body Simulations of Disks

Published online by Cambridge University Press:  14 August 2015

F. Hohl
F. Hohl*
Affiliation:
NASA, Langley Research Center, Hampton, Va., U.S.A.

Abstract

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The methods used in the large-scale n-body simulations are discussed. However, the present review concentrates on the results already obtained in the n-body simulations using systems containing up to 200000 simulation stars. Results are presented which show that the stability criterion developed for flattened systems applies only to truly axisymmetric instabilities. Purely stellar disks acquire rather large velocity dispersions, generally two or more times the velocity dispersion required by Toomre for axisymmetric stability. In the computer simulations, the bar-forming instability can be prevented only by comparatively large velocity dispersions. However, simulations inclusing the effects of the galactic halo and core as a fixed background field show that bar formation can be prevented for fixed halo components as large or larger than the self-consistent disk component. Experiments performed to determine the collisional relaxation time for the large-scale gravitational n-body calculations show that these models are indeed ‘collisionless’.

Type
Part II/Flattened Systems
Information
Symposium - International Astronomical Union , Volume 69: Dynamics of Stellar Systems , 1975 , pp. 349 - 366
Copyright
Copyright © Reidel 1975 

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