On density waves in galaxies. V - Maintenance of spiral structure and discrete spiral modes

Details On density waves in galaxies. V - Maintenance of spiral structure and discrete spiral modes On density waves in galaxies. V - Maintenance of spiral structure and discrete spiral modes

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...212..645m&link_type=abstract

Astrophysical Journal, Part 1, vol. 212, Mar. 15, 1977, p. 645-658.

Astronomy and Astrophysics

Astrophysics

32

Density Wave Model, Galactic Structure, Hydrodynamics, Spiral Galaxies, Stellar Motions, Angular Momentum, Astrophysics, Boundary Value Problems, Resonance, Star Distribution, Wave Reflection, Wentzel-Kramer-Brillouin Method

Scientific paper

This paper substantiates earlier suggestions that the maintenance and excitation of spiral structures in galaxies can occur via spiral modes which are dominated by the dynamics of stellar motions within a galactic disk. A physical derivation, certain numerical results, and some general properties are presented for that type of spiral mode which involves 'feedback' and consists of temporally growing spiral waves that rotate rigidly about the galactic center with a fixed-pattern rotation frequency. The discrete values of allowed pattern frequencies are determined through a global dispersion relationship in the form of a standing-wave condition, this condition is evaluated in terms of the radial wavenumber throughout an annular region between two galactocentric reflection circles, and growth rates of the spiral modes are computed. A numerical example is given for a galaxy model with a total mass of 20 billion solar masses and a rotation curve typical of galaxies with a low central concentration of matter.

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