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Instabilities of Stellar Systems in Near-Keplerian and Near-Harmonic Potentials


E.V. Polyachenko

Stability of selfgravitating stellar clusters of razor-thin disk and spherical geometry in external dominaating gravitational potential is considered, providing that the potential is due to massive black hole or almost homogeneous heavy halo of dark matter. Both potentials allow one to simplify the general problem reducing it to the problem of stability of interacting stellar orbits. There are two instabilities in radially anisotropic models of stellar systems: radial orbit instability and gravitational loss-cone instability

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