Abstract
Many simulations of disc galaxies exhibit a succession of transient spiral patterns when sufficient halo is included to suppress the global bar instability (Hohl 1970, Hockney and Brownrigg 1974, Sellwood and James 1979). This behaviour causes the velocity dispersion to rise secularly which in turn reduces the intensity of the patterns. Spiral activity usually ceases altogether as Q tends asymptotically to a value somewhat greater than 2.
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References
Hockney, R.W. & Brownrigg, D.R.K. (1974) M.N.R.A.S. 167, 351.
Hohl, F. (1970) NASA TR R-343.
Sellwood, J.A. & James, R.A. (1979) M.N.R.A.S. 187, 485.
Toomre, A. (1981) “Normal Galaxies” Eds. Fall, S.M. & Lynden-Bell, D. Cambridge Univ. Press.
Wielen, R. (1974), Highlights of Astronomy 3, 395.
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© 1983 IAU
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Carlberg, R.G., Sellwood, J.A. (1983). Spiral Instabilities and Disc Heating. In: Athanassoula, E. (eds) Internal Kinematics and Dynamics of Galaxies. International Astronomical Union/Union Astronomique Internationale, vol 100. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7075-5_32
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DOI: https://doi.org/10.1007/978-94-009-7075-5_32
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