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Dynamical evolution of dense star clusters in galactic nuclei

Published online by Cambridge University Press:  22 May 2014

Jaroslav Haas  and
Ladislav Šubr
Jaroslav Haas
Affiliation:
Charles University in Prague, Faculty of Mathematics and Physics, V Holešovičkách 2, 18000, Prague, Czech Republic email: haas@sirrah.troja.mff.cuni.cz, subr@sirrah.troja.mff.cuni.cz
Ladislav Šubr
Affiliation:
Charles University in Prague, Faculty of Mathematics and Physics, V Holešovičkách 2, 18000, Prague, Czech Republic email: haas@sirrah.troja.mff.cuni.cz, subr@sirrah.troja.mff.cuni.cz
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Abstract

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By means of direct numerical N-body modeling, we investigate the orbital evolution of an initially thin, central mass dominated stellar disk. We include the perturbative gravitational influence of an extended spherically symmetric star cluster and the mutual gravitational interaction of the stars within the disk. Our results show that the two-body relaxation of the disk leads to significant changes of its radial density profile. In particular, the disk naturally evolves, for a variety of initial configurations, a similar broken power-law surface density profile. Hence, it appears that the single power-law surface density profile ∝R−2 suggested by various authors to describe the young stellar disk observed in the Sgr A* region does not match theoretical expectations.

Keywords

methods: n-body simulationsstellar dynamicsGalaxy: nucleus
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S303: The Galactic Center: Feeding and Feedback in a Normal Galactic Nucleus , October 2013 , pp. 235 - 237
Copyright
Copyright © International Astronomical Union 2014 

References

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