The stellar distribution around a black hole - Numerical integration of the Fokker-Planck equation

Details The stellar distribution around a black hole - Numerical integration of the Fokker-Planck equation The stellar distribution around a black hole - Numerical integration of the Fokker-Planck equation

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...226.1087c&link_type=abstract

Astrophysical Journal, Part 1, vol. 226, Dec. 15, 1978, p. 1087-1108.

Astronomy and Astrophysics

Astronomy

128

Black Holes (Astronomy), Fokker-Planck Equation, Numerical Integration, Star Distribution, Stellar Motions, Boundary Layer Equations, Collision Parameters, Density Distribution, Diffusion Coefficient, Distribution Functions, Globular Clusters, Monte Carlo Method, Plasma Loss, Star Clusters, Steady State, Velocity Distribution

Scientific paper

The steady-state stellar distribution around a central black hole in a star cluster is determined by means of a direct numerical integration of the Fokker-Planck equation in energy-angular momentum space. The loss cone in phase space resulting from tidal destruction of stars is treated by means of a detailed boundary-layer analysis. The process of stellar destruction by direct physical collisions is treated by use of the physical collision cross section. The two-dimensional steady-state distribution function, the density and velocity dispersion profiles of the stellar distribution, and stellar consumption rates are presented for black holes in globular cluster environments. The distribution function obtained is in reasonable agreement with that resulting from the Monte Carlo simulations of Shapiro and Marchant (1978); the present loss rate is larger than theirs by a factor of 2.

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