Density wave theory for spiral galaxies - The regime of finite spiral arm inclination in stellar dynamics

Details Density wave theory for spiral galaxies - The regime of finite spiral arm inclination in stellar dynamics Density wave theory for spiral galaxies - The regime of finite spiral arm inclination in stellar dynamics

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....64..389b&link_type=abstract

Astronomy and Astrophysics, vol. 64, no. 3, Mar. 1978, p. 389-397. Research supported by the European Space Agency

Astronomy and Astrophysics

Astrophysics

24

Density Wave Model, Spiral Galaxies, Stellar Motions, Angular Momentum, Astronomical Models, Differential Equations, Self Excitation, Wave Amplification

Scientific paper

Provided that the disk stars have moderately small epicycles, an appropriate asymptotic solution can be obtained for the stellar dynamic equations governing wave phenomena in thin disk galaxies. The major new astrophysical effect of this regime is an enhanced amplification of spiral density waves near their region of corotation with the disk stars. The basic mechanism for amplification is still related to an outward transport of angular momentum. Nevertheless, as a tool for the study of spiral waves in galaxies, the asymptotic solutions have wider applicability than those where the spiral inclination is more strongly restricted. Also briefly illustrated are the finite inclination effects for several spiral modes in realistic galaxy models. The wave amplification results in a fairly rapid growth of such global modes from noise to observable amplitudes in some billion yr or less. The stellar dynamic growth rates are typically about twice as large as those previously estimated by a gaseous model.

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