Hostname: page-component-7479d7b7d-pfhbr Total loading time: 0 Render date: 2024-07-12T00:51:11.585Z Has data issue: false hasContentIssue false
  • English
  • Français

Spiral Instabilities and Disc Heating

Published online by Cambridge University Press:  04 August 2017

R. G. Carlberg  and
J. A. Sellwood
R. G. Carlberg
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA.
J. A. Sellwood
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
II. Spiral Structure
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 127 - 128
Copyright
Copyright © Reidel 1983 

References

Hockney, R.W. & Brownrigg, D.R.K. (1974) M.N.R.A.S. 167, 351.Google Scholar
Hohl, F. (1970) NASA TR R-343.Google Scholar
Sellwood, J.A. & James, R.A. (1979) M.N.R.A.S. 187, 485.Google Scholar
Toomre, A. (1981) “Normal Galaxies” Eds. Fall, S.M. & Lynden-Bell, D. Cambridge Univ. Press.Google Scholar
Wielen, R. (1974), Highlights of Astronomy 3, 395.Google Scholar