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Intermediate-Mass Black Holes in binary rich star clusters

Published online by Cambridge University Press:  11 March 2020

Ladislav Šubr Open the ORCID record for Ladislav Šubr [Opens in a new window] ,
Giacomo Fragione Open the ORCID record for Giacomo Fragione [Opens in a new window]  and
Jörg Dabringhausen Open the ORCID record for Jörg Dabringhausen [Opens in a new window]
Ladislav Šubr
Affiliation:
Astronomical Institute, Charles University, Prague, Czech Republic
Giacomo Fragione
Affiliation:
Racah Institute for Physics, The Hebrew University, Jerusalem, Israel
Jörg Dabringhausen
Affiliation:
Astronomical Institute, Charles University, Prague, Czech Republic
Rights & Permissions [Opens in a new window]

Abstract

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Three-body interactions of stellar-mass binaries with intermediate mass black holes (IMBHs) in nuclei of globular clusters may produce specific features that may serve as an independent indicator of existence of the IMBHs. By means of direct N-body integrations we follow the dynamical evolution of globular clusters of moderate extension and mass with 50% binary population over a time span of ≍ 0.8 Gyr and compare the cases with and without the primordial binaries as well as with and without the IMBH. We show that (i) presence of the IMBH leads to rapid formation of a density cusp regardless of the initial binary fraction, (ii) binary rich clusters with the IMBH produce high velocity escapers at a rate of ≍ 0.1 Myr−1 and (iii) clusters hosting an IMBH together with high number of binaries form a denser halo of marginally unbound stars than clusters that lack either the IMBH or the binary population.

Keywords

stellar dynamicsglobular clusters: generalbinaries: generalmethods: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 520 - 523
Copyright
© International Astronomical Union 2020

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