paper

On strong mass segregation around a massive black hole: Implications for lower-frequency gravitational-wave astrophysics

arXiv:0910.3206 · doi:10.1088/2041-8205/708/1/L42

Abstract

We present, for the first time, a clear -body realization of the {\it strong mass segregation} solution for the stellar distribution around a massive black hole. We compare our -body results with those obtained by solving the orbit-averaged Fokker-Planck (FP) equation in energy space. The -body segregation is slightly stronger than in the FP solution, but both confirm the {\it robustness} of the regime of strong segregation when the number fraction of heavy stars is a (realistically) small fraction of the total population. In view of recent observations revealing a dearth of giant stars in the sub-parsec region of the Milky Way, we show that the time scales associated with cusp re-growth are not longer than . These time scales are shorter than a Hubble time for black holes masses $\mbul \lesssim 4 \times 10^6 M_\odot$ and we conclude that quasi-steady, mass segregated, stellar cusps may be common around MBHs in this mass range. Since EMRI rates scale as $\mbul^{-α}$, with $α\in [1\4,1]$, a good fraction of these events should originate from strongly segregated stellar cusps.

5 pages, 4 figures, 1 table, submitted to ApJL

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