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The Global Stability of our Galaxy

Published online by Cambridge University Press:  04 August 2017

J. A. Sellwood
J. A. Sellwood*
Affiliation:
Kapteyn Laboratory, Groningen

Extract

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Many mass models of our Galaxy (see e.g. Schmidt 1985 for a review) assume the disc to be nearly axisymmetric. For consistency, therefore, no such model should possess gross non-axisymmetric instabilities. However, most attribute less than half the central attraction at the Sun to bulge and halo material - a situation where bar forming instabilities are frequently found (see e.g. Sellwood 1983).

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 117: Dark Matter in the Universe , 1987 , pp. 301
Copyright
Copyright © Reidel 1987 

References

Bahcall, J.N., Schmidt, M. and Soniera, R. (1982) Ap. J. Lett. 258, L23.CrossRefGoogle Scholar
Schmidt, M. (1985) The Milky Way Galaxy, IAU Symposium 106, eds. van Woerden, H., Allen, R.J. and Burton, W.B., Reidel.Google Scholar
Sellwood, J.A. (1983) Internal Kinematics and Dynamics of Galaxies, IAU Symposium 100, ed. Athanassoula, E., Reidel.Google Scholar
Sellwood, J.A. (1985) MNRAS, 216, in press.Google Scholar
Toomre, A. (1981) Structure and Evolution of Normal Galaxies, eds. Fall, S.M. and Lynden-Bell, D., Cambridge University Press.Google Scholar