The Kinematic Richness of Star Clusters - II. Stability of Spherical Anisotropic Models with Rotation

Philip G. Breen, Simon Rozier, Douglas C. Heggie*, Anna Lisa Varri

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

We study the bar instability in collisionless, rotating, anisotropic, stellar systems, using N-body simulations and also the matrix technique for calculation of modes with the perturbed collisionless Boltzmann equation. These methods are applied to spherical systems with an initial Plummer density distribution, but modified kinematically in two ways: the velocity distribution is tangentially anisotropic, using results of Dejonghe, and the system is set in rotation by reversing the velocities of a fraction of stars in various regions of phase space, a la Lynden-Bell. The aim of the N-body simulations is first to survey the parameter space, and, using those results, to identify regions of phase space (by radius and orbital inclination) which have the most important influence on the bar instability. The matrix method is then used to identify the resonant interactions in the system which have the greatest effect on the growth rate of a bar. Complementary series of N-body simulations examine these processes in relation to the evolving frequency distribution and the pattern speed. Finally, the results are synthesised with an existing theoretical framework, and used to consider the old question of constructing a stability criterion.
Original languageEnglish
Pages (from-to)4762-4778
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
Early online date9 Feb 2021
Publication statusPublished - 1 Apr 2021

Keywords / Materials (for Non-textual outputs)

  • astro-ph.GA


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