Contributions to the theory of spiral structure. III - The influence of homogeneous and inhomogeneous halos on the equilibrium and stability of disk galaxies

Details Contributions to the theory of spiral structure. III - The influence of homogeneous and inhomogeneous halos on the equilibrium and stability of disk galaxies Contributions to the theory of spiral structure. III - The influence of homogeneous and inhomogeneous halos on the equilibrium and stability of disk galaxies

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....82..238s&link_type=abstract

Astronomy and Astrophysics, vol. 82, no. 1-2, Feb. 1980, p. 238-243.

Physics

Fluid Dynamics

1

Astronomical Models, Disk Galaxies, Dynamic Stability, Halos, Spirals, Dynamic Models, Equilibrium, Fluid Dynamics

Scientific paper

By fluid-dynamical calculations it can be shown that disk-like figures of equilibrium exist inside homogeneous and inhomogeneous galactic halos. The range of possible axial ratios of the spheroidal disk component is closely related to the ratio of halo to disk density, insofar as the flattening of the disk is confined to a region between c/a = 0 and (c/a)max, which decreases with increasing density ratio. By applying classical methods it can be demonstrated how the surrounding halo is able to stabilize flattened disks against ellipsoidal deformations, if the halo density is large enough. The critical axial ratio for secular stability is reduced from c/a = 0.58 to 0.3 if the central halo density exceeds that of the disk by a factor of 1.5, whereas the dynamical instability can be totally removed by halos of much smaller density.
Comparing our results with recent numerical models we find that the halo density of our galaxy does not seem to be large enough to render the galactic disk secularly stable. Finally a possibility to generalize the problem for the case of real stellar disks and to describe stellar systems by figures of equilibrium is outlined.

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