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The theory of spiral structure of galaxies
Published online by Cambridge University Press: 14 August 2015
Abstract
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A Landau-type instability mechanism for generating spiral waves is suggested.
Two populations of stars, Populations I and II, are considered, the second one with mean rotational velocity zero. Then a dispersion relation is derived which is reduced to the Lin-Shu dispersion relation in the case of vanishing Population II. The amplification of the wave is of the same type as the two-stream instability. It occurs if the angular velocity of the spiral pattern Ωs is smaller than the angular velocity of the Population I stars. A value of Ωs = 22–25 km s−1 kpc−1 was found, as well as the growth parameter. Spiral arms are formed in 108–109 yr, while trailing and leading waves grow at the same rate.
A quasi-linear theory is developed to account for the limited growth of the spiral waves.
Detailed accounts of the theory and of its implications are contained in recent publications (Marochnik, 1969; Marochnik and Suchkov, 1969a; 1969b; Marochnik and Ptitzina, 1969; Marochnik et al., 1969).
- Type
- Part III/Theory of Spiral Structure
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- Copyright
- Copyright © Reidel 1970
References
Marochnik, L. S., Pomagaev, S. G., Sagdeev, R. Z., and Suchkov, A. A.: 1969, Dokl. Akad. Nauk S.S.S.R., in press.Google Scholar
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