Physics – Fluid Dynamics
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...108..265b&link_type=abstract
Astronomy and Astrophysics, vol. 108, no. 2, Apr. 1982, p. 265-273. Research supported by the Consiglio Nazionale delle Ricerch
Physics
Fluid Dynamics
4
Density Wave Model, Galactic Structure, Spiral Galaxies, Stellar Rotation, Angular Momentum, Astronomical Models, Asymptotic Methods, Differential Equations, Energy Transfer, Fluid Dynamics, Momentum Transfer, Resonance
Scientific paper
Density wave theory has already shown that galaxy disks can support discrete self-excited spiral modes independently of resonant effects at corotation. However, in the problem of excitation of spiral modes in more general galaxy models, and especially in the mechanism for selection of the prominent structures, energy and angular momentum exchange with the corotating stars might play an important role. In order to study these resonant effects and give a quantitative discussion of their importance, we improve the simple asymptotic differential equation that was previously used to calculate spiral modes. We find that the stellar dynamic evaluation of the resonant contribution is quite different from what was argued previously on the basis of a fluid model. Generally, in realistic galaxy models resonant effects at corotation are less important than expected.
Bertin Giuseppe
Haass J.
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