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%arXiv:0909.1318
\documentstyle{article}
\begin{document}
\title{The Distribution of Stars and Stellar Remnants at the Galactic 
Center}
\author{David Merritt}
\affil{Department of Physics and Center for Computational Relativity and
Gravitation, Rochester Institute of Technology, Rochester, NY 14623, USA}
\begin{abstract}
Motivated by recent observations that suggest a low density of old
stars around the Milky Way supermassive black hole, evolutionary
models for the nuclear star cluster are considered that postulate
a parsec-scale core as initial conditions.
Gravitational encounters cause the core to shrink;
a core of initial radius $1-1.5$ pc evolves to a size of
$0.5$ pc after $10$ Gyr, roughly the size of the observed core.
The absence of a Bahcall-Wolf cusp is naturally explained.
In these models, the time for a $10\msun$ black hole to spiral in to the
Galactic center from an initial distance of $5$ pc
can be much greater than $10$ Gyr.
Assuming that the stellar black holes had the same phase-space distribution
initially as the stars, their density after $5-10$ Gyr is predicted
to rise very steeply going into the stellar core, but to remain
substantially below the densities inferred from steady-state
models that include a steep density cusp in the stars.
The implications of these models are discussed for the rates of
gravitational-wave inspiral events and of other physical processes that 
depend
on a high density of stars or stellar mass black holes near \sgr.
\end{abstract}
\end{document}

-- 
David MERRITT
Department of Physics
85 Lomb Memorial Drive
Rochester Institute of Technology
Rochester, NY 14623-5604
Phone: 585-475-7973
Web: http://ccrg.rit.edu/people/merritt/
E-mail: merritt@astro.rit.edu