Physics
Scientific paper
May 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012apj...750...31u&link_type=abstract
The Astrophysical Journal, Volume 750, Issue 1, article id. 31 (2012).
Physics
Black Hole Physics, Globular Clusters: General, Globular Clusters: Individual: Ngc 5694, Methods: Numerical, Stars: Kinematics And Dynamics
Scientific paper
We present results from a series of Monte Carlo (MC) simulations investigating the imprint of a central intermediate-mass black hole (IMBH) on the structure of a globular cluster. We investigate the three-dimensional and projected density profiles, and stellar disruption rates for idealized as well as realistic cluster models, taking into account a stellar mass spectrum and stellar evolution, and allowing for a larger, more realistic number of stars than was previously possible with direct N-body methods. We compare our results to other N-body and Fokker-Planck simulations published previously. We find, in general, very good agreement for the overall cluster structure and dynamical evolution between direct N-body simulations and our MC simulations. Significant differences exist in the number of stars that are tidally disrupted by the IMBH, and this is most likely caused by the wandering motion of the IMBH, not included in the MC scheme. These differences, however, are negligible for the final IMBH masses in realistic cluster models, as the disruption rates are generally much lower than for single-mass clusters. As a direct comparison to observations we construct a detailed model for the cluster NGC 5694, which is known to possess a central surface brightness cusp consistent with the presence of an IMBH. We find that not only the inner slope but also the outer part of the surface brightness profile agree well with observations. However, there is only a slight preference for models harboring an IMBH compared to models without.
Chatterjee Sourav
Fregeau John M.
Rasio Frederic A.
Umbreit Stefan
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