Self-similar Gravitational Collapse in Stellar Dynamics

Details Self-similar Gravitational Collapse in Stellar Dynamics Self-similar Gravitational Collapse in Stellar Dynamics

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...549l..93l&link_type=abstract

The Astrophysical Journal, Volume 549, Issue 1, pp. L93-L96.

Astronomy and Astrophysics

Astronomy

15

Celestial Mechanics, Stellar Dynamics, Galaxies: Star Clusters, Galaxy: Globular Clusters: General

Scientific paper

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 ρ(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.

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