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The steady-state distribution of stars around a massive black hole in a globular cluster is determined by solving numerically the coupled time-dependent Boltzmann equations for a system containing stars of two different masses. Similar results are found for an arbitrary spectrum of masses with the aid of approximate analytic solutions of the time-independent equations. The effects of mass segregation are summarized by scaling laws that are derived both by analytic approximations and by numerical solutions. The detectability of a black hole in a globular cluster is discussed in terms of possible observations of the central star distributions.
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Bahcall et al. (1977) studied this question.
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