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Bending Instability in A Rotating Stellar Disk
並列摘要
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. I present a high resolution particle simulation with particle number N = 3,000,000, and discover that the bending instability can be driven by moderately anisotropic velocity dispersion of stars, even without a bar in the center of 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 a important parameter for bending instability in a rotating system.
並列關鍵字
無資料延伸閱讀
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