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 mass-segr.tex ApJ, Mar 2006, submitted
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% astro-ph/0603280

\documentclass[12pt,preprint,letter]{aastex}

\begin{document}

\title{Stellar remnants in galactic nuclei: mass segregation.}

\author{Marc Freitag\altaffilmark{1,2}\thanks{e-mail: freitag@ast.cam.ac.uk},
Pau Amaro-Seoane\altaffilmark{3} and

\altaffiltext{1}{Department of Physics and Astronomy,
Northwestern University, Evanston, IL 60208, USA}
\altaffiltext{2}{Institute of Astronomy, University of Cambridge,
Madingley Road, CB3~0HA Cambridge, UK}
\altaffiltext{3}{Max Planck Intitut f\"ur Gravitationsphysik
(Albert-Einstein-Institut), D-14476 Potsdam, Germany}

\begin{abstract}
The study of how stars distribute themselves around a massive black
hole (MBH) in the center of a galaxy is an important prerequisite for
the understanding of many galactic-center processes.  These include
the observed overabundance of point X-ray sources at the Galactic
center, the prediction of rates and characteristics of tidal
disruptions of extended stars by the MBH and of inspirals of compact
stars into the MBH, the latter being events of high importance for the
future space borne gravitational wave interferometer LISA. In
relatively small galactic nuclei, hosting MBHs with masses in the
range $10^5-10^7\,M_\odot$, the single most important dynamical
process is 2-body relaxation. It induces the formation of a steep
density cusp around the MBH and strong mass segregation, as more
massive stars lose energy to lighter ones and drift to the central
regions. Using a spherical stellar dynamical Monte-Carlo code, we
simulate the long-term relaxational evolution of galactic nucleus
models with a spectrum of stellar masses. Our focus is the
concentration of stellar black holes to the immediate vicinity of the
MBH. We quantify this mass segregation for a variety of galactic
nucleus models and discuss its astrophysical implications. Special
attention is given to models developed to match the conditions in the
Milky Way nucleus; we examine the presence of compact objects in
connection to recent high-resolution X-ray observations.
\end{abstract}

\end{document}