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Effects of Stellar-Mass Black Holes on Massive Star Cluster Evolution

Published online by Cambridge University Press:  31 March 2017

Sourav Chatterjee ,
Meagan Morscher ,
Carl L. Rodriguez ,
Bharat Pattabiraman  and
Frederic A. Rasio
Sourav Chatterjee
Affiliation:
Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA email: sourav.chatterjee@northwestern.edu
Meagan Morscher
Affiliation:
Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA email: sourav.chatterjee@northwestern.edu
Carl L. Rodriguez
Affiliation:
Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA email: sourav.chatterjee@northwestern.edu
Bharat Pattabiraman
Affiliation:
Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA email: sourav.chatterjee@northwestern.edu
Frederic A. Rasio
Affiliation:
Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA email: sourav.chatterjee@northwestern.edu
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Abstract

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Recent observations have revealed the existence of stellar mass black hole (BH) candidates in some globular clusters (GC) in the Milky Way and in other galaxies. Given that the detection of BHs is challenging, these detections likely indicate the existence of large populations of BHs in these clusters. This is in direct contrast to the past understanding that at most a handful of BHs may remain in old GCs due to quick mass segregation and rapid mutual dynamical ejection. Modern realistic star-by-star numerical simulations suggest that the retention fraction of BHs is typically much higher than what was previously thought. The BH dynamics near the cluster center leads to dynamical formation of new binaries and dynamical ejections, and acts as a persistent and significant energy source for these clusters. We have started exploring effects of BHs on the global evolution and survival of star clusters. We find that the evolution as well as survival of massive star clusters can critically depend on the details of the initial assumptions related to BH formation physics, such as natal kick distribution, and the initial stellar mass function (IMF). In this article we will present our latest results.

Keywords

black hole physics–stellar dynamics–methods: n-body simulations–methods: numerical–globular clusters: general–kinematics and dynamics–galaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S316: Formation, evolution, and survival of massive star clusters , August 2015 , pp. 234 - 239
Copyright
Copyright © International Astronomical Union 2017 

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