Bending instability in a rotating stellar disk.

Details Bending instability in a rotating stellar disk. Bending instability in a rotating stellar disk.

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000chjph..38..111t&link_type=abstract

Chin. J. Phys., Vol. 38, No. 2, p. 111 - 119

Physics

2

Galactic Disks: Numerical Simulations, Stellar Disks: Perturbations

Scientific paper

Most simulations on bending instability adopt the particle-mesh scheme and lack resolution in the direction normal to the disk plane, which can lead to suppression of the bending instabilities. The author presents a high resolution particle simulation with particle number N = 3,000,000, and discovers that the bending instability can be driven by moderately anisotropic velocity dispersion of stars, even without a bar in the center of the galaxy or a counter-rotating stellar disk. The simulation results show that a rigidly rotating disk can be unstable to bending perturbations, with the Toomre's Q value equal to 1.3 and the velocity anisotropy σz/σh equal to 1/√2. Besides the velocity anisotropy, the Toomre's Q value is also an important parameter for the bending instability in a rotating system.

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