## Abstract

Self-similar gravitational collapse of a globular cluster is studied using the nonlinear kinetic standard model of stellar dynamics consisting of the Fokker-Planck-Vlasov transport equation coupled self-consistently to Poisson's equation for the Newtonian gravitational potential. It is shown rigorously that any locally integrable self-similar solution to these equations must approach a mass density profile p(r, t) ∝ r^{-α}, α = 3, in the final stage of the collapse. The discrepancy between the exact value α = 3 and previous results in the range 2 < α < 2.5 obtained from the orbit-averaged approximation to the kinetic model raises some questions about the validity of this popular approximation.

Original language | English (US) |
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Pages (from-to) | L93-L96 |

Journal | Astrophysical Journal |

Volume | 549 |

Issue number | 1 PART 2 |

DOIs | |

State | Published - Mar 1 2001 |

## All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

## Keywords

- Celestial mechanics, stellar dynamics
- Galaxies: Star clusters
- Globular clusters: General