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The Global Stability of our Galaxy

  • J. A. Sellwood (a1)

Extract

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).

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Copyright

References

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

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