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Tightly Wound Spirals

We assume the wave driven by the self-gravity has a form of tightly-wound spiral [Fig.3.3(left)]. When we move radially, the density varies rapidly. While, it changes its amplitude slowly in the azimuthal direction. In a mathematical expression, if we write the density perturbation as
 (3.21)

where the amplitude of spiral is a slowly varing function of , a tightly wound spiral means the shape function varies fast (the radial wavenumber is large enough). We consider the gravitational force from the vicinity of , since the oscillates and cancels even if we integrate over large region. Thus,
 (3.22)

where
 (3.23)

Notice that the density perturbation [eq.(3.22)] is similar to that studied in 2.6. The potential should be expressed in a similar form to equation (2.64) as
 (3.24)

which simply means
 (3.25)

If we set , we obtain our final result for the potential due to the surface density perturbation
 (3.26)

Differentiating this equation with and ignoring the term compared to that of , we obtain
 (3.27)

Neglecting the terms compared to the terms containing , equations (3.18), (3.19), and (3.20) are rewritten as
 (3.28)

 (3.29)

and
 (3.30)

Using these equations [(3.28), (3.29), and (3.30)], , and , we obtain the dispersion relation for the self-gravitating instability of the rotating gaseous thin disk
 (3.31)

Generally speaking, the epicyclic frequency depends on the rotation law but is in the range of (see Table 3.1 for for typical rotation laws). It is shown that the system is stabilized due to the epicyclic frequency compared with a nonrotating thin disk [eq.(2.65)].

 Rotation Rigid-body rotation const. Flat rotation const. Kepler rotation

Next: Toomre's Value Up: Gravitational Instability of Rotating Previous: Gravitational Instability of Rotating   Contents
Kohji Tomisaka 2007-07-08