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Instabilities of Hot Stellar Discs

Published online by Cambridge University Press:  04 August 2017

E. Athanassoula  and
J. A. Sellwood
E. Athanassoula
Affiliation:
Observatoire de Besancon, 25000 Besancon, France. Institute of Astronomy, Madingley Road, Cambridge, England.
J. A. Sellwood
Affiliation:
Observatoire de Besancon, 25000 Besancon, France. Institute of Astronomy, Madingley Road, Cambridge, England.

Extract

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We use computer simulations to determine the dominant unstable modes of stellar discs having the surface density distribution of Toomre's (1963) model 1 and large random motions in the plane. Particles in the models have their initial coordinates chosen from distribution functions to ensure that the configurations would, in the limit of infinitely many particles, be stationary solutions of the Vlasov and Poisson equations. The 40,000 particles in our simulations are constrained to move on a plane and we use a polar grid based Fourier method to determine the force field (Sellwood 1982). The surface density is smoothly tapered to zero at six scale lengths and the softening length is 1/30th of the outer radius of the disc.

Type
IV. Barred Galaxies
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 203 - 204
Copyright
Copyright © Reidel 1983 

References

Kalnajs, A.J.: 1976, Ap. J. 205, 751.CrossRefGoogle Scholar
Sellwood, J.A.: 1982, J. Comp. Phys. (in press).Google Scholar
Toomre, A.: 1963, Ap. J. 138, 385.Google Scholar