Dynamical stability of differentially rotating masses. III - Additional numerical results and interpretation

Details Dynamical stability of differentially rotating masses. III - Additional numerical results and interpretation Dynamical stability of differentially rotating masses. III - Additional numerical results and interpretation

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.248..256l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 248, Jan. 15, 1991, p. 256-271.

Statistics

Computation

2

Computational Astrophysics, Dynamic Stability, Rotating Matter, Astronomical Models, Equilibrium Equations, Perturbation Theory, Rotating Cylinders

Scientific paper

The dynamical stability of differentially rotating, self-gravitating masses is investigated. Two types of shear instability are obtained. The first is caused by the 'principal' mode which is characterized by a peak growth rate and large azimuthal wavenumbers. This mode disappears for large shear or large flattening. It is shown that this instability can be described in terms of two parameters. The m = 2 principal mode achieves a nonlinear evolution from an initially axisymmetric state toward a uniformly rotating Jacobi ellipsoid. The second type of instability is related to the 'secondary' modes. They form a discrete spectrum of corotating modes. They have a smaller growth rate than the principal mode for low values of m. Larger growth rates are obtained for large m. In the case of a flattened disk, it is shown that these modes can be identified with the unstable acoustic waves which are known to occur in compressible shear flows.

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