CURVATURE AND ACOUSTIC INSTABILITIES IN ROTATING FLUID DISKS

摘要

The stability of a rotating fluid disk to the formation of spiral arms is studied in the tight-winding approximation in the linear regime. The dispersion relation for spirals that was derived by Bertin et al. is shown to contain a new, acoustic instability beyond the Lindblad resonances that depends only on pres- sure and rotation. In this regime, pressure and gravity exchange roles as drivers and inhibitors of spiral wave structures. Other instabilities that are enhanced by pressure are also found in the general disper- sion relation by including higher order terms in the small parameter l/kr for wavenumber k and radius r. We identify two important dimensionless physical parameters: #EPSILON# = 2 PI G DELTA O/(rK~2), which is essentially the ratio of disk mass to total mass (disk and halo), and a/(kr), which is the ratio of epicyclic radius to disk radius (delta o is the mass column density, k is the epicyclic frequency, and a is the sound speed). The small term zeta = (k~2r~2 + m~2)-1/2 is an additional parameter that is purely geometrical for number of arms m. When these terms are included in the dispersion relation, the oscillation frequency becomes complex, leading to the growth of perturbations even for large values of Toomre's parameter Q. The growth rate is proportional to a linear combination of terms that depend on e and a/(kr). Instabilities that arise from e are termed gravitational-curvature instabilities because epsilon depends on the disk mass and is largest when the radius is small, i.e., when the orbital curvature is large. Instabilities that arise from a/