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 mn.tex arXiv:1004.2703
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%arXiv:1004.2703
%http://adsabs.harvard.edu/abs/2010arXiv1004.2703P

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\begin{document}
\shorttitle{Origin of the B-stars in the Galactic center}
\shortauthors{Perets \& Gualandris}
\title{Dynamical constraints on the origin of the young B-stars in the 
Galactic
center}


\author{Hagai B. Perets\altaffilmark{1} and Alessia 


\altaffiltext{1}{CfA fellow, Harvard-Smithsonian Center for 
Astrophysics, 60 Garden St., Camridge, MA 02138, USA}

\altaffiltext{2}{Max-Planck Institut f<FC>r Astrophysik, 
Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany}

\begin{abstract}
Regular star formation is thought to be inhibited close to the massive
black hole (MBH) in the Galactic center. Nevertheless, tens of young
main sequence B stars have been observed in an isotropic distribution
close to it. These stars are observed to have an apparently continuous
distribution from very close to the MBH $<0.01$ pc and up to at least
$\sim0.5$ pc, suggesting a common origin. Various models have been
suggested for the formation of the B-stars closest to the MBH ($<0.05$
pc; the S-stars), typically involving the migration of these stars
from their original birthplace to their currently observed position.
Here we explore the orbital phase space distribution of the B-stars
throughout the central $pc$ expected from the various suggested models
for the origin of the B-stars. We find that most of these models have
difficulties in explaining, by themselves, both the population of
the S-stars ($<0.05$ pc), and the population of the young B-stars
further away (up to $0.5$ pc). Most models grossly over-predict the
number of B-stars up to $0.5$ pc, given the observed number of S-stars.
Such models include the intermediate-mass black hole assisted cluster
inspiral scenario, Kozai-like perturbations by two disks, spiral density
waves migration in a gaseous disk, and some of the eccentric disk
instability models. We focus on one of the other models, the massive
perturber induced binary disruption, which is consistent with both
the S-stars and the extended population of B-stars further away. For
this model we use analytical arguments and N-body simulations to provide
further observational predictions. These could be compared with future
observations to further support this model, constrain it or refute
it. These predictions include the radial distribution of the young
B-stars, their eccentricity distribution and its dependence on distance
from the MBH (higher eccentricities at larger distances from the MBH),
as well as less specific expectations regarding their mass function.
\end{abstract}
|\end{document}|

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fn:Hagai Perets
n:Perets;Hagai
org:Harvard-Smithsonian Center for Astrophysics;Institute for Theory and Computation (ITC)
adr:Camrdige, MA;;60 Garden St.;Cambridge;MA;02138;USA
email;internet:hperets@cfa.harvard.edu
title:CfA fellow
tel;work:1+617-4962575
tel;cell:1+617-8777030
url:http://www.cfa.harvard.edu/~hperets/index.html
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