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The Role of “black hole burning” in the evolution of dense star clusters

Published online by Cambridge University Press:  11 March 2020

Kyle Kremer Open the ORCID record for Kyle Kremer [Opens in a new window] ,
Claire S. Ye Open the ORCID record for Claire S. Ye [Opens in a new window] ,
Sourav Chatterjee ,
Carl L. Rodriguez  and
Frederic A. Rasio
Kyle Kremer
Affiliation:
Department of Physics & Astronomy and Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA email: kremer@northwestern.edu
Claire S. Ye
Affiliation:
Department of Physics & Astronomy and Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA email: kremer@northwestern.edu
Sourav Chatterjee
Affiliation:
Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai400005, India
Carl L. Rodriguez
Affiliation:
MIT-Kavli Institute for Astrophysics and Space Research, Cambridge, MA02139, USA
Frederic A. Rasio
Affiliation:
Department of Physics & Astronomy and Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA email: kremer@northwestern.edu
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Abstract

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As self-gravitating systems, dense star clusters exhibit a natural diffusion of energy from their innermost to outermost regions, leading to a slow and steady contraction of the core until it ultimately collapses under gravity. However, in spite of the natural tendency toward “core collapse,” the globular clusters (GCs) in the Milky Way exhibit a well-observed bimodal distribution in core radii separating the core-collapsed and non-core-collapsed clusters. This suggests an internal energy source is at work, delaying the onset of core collapse in many clusters. Over the past decade, a large amount of work has suggested that stellar black holes (BHs) play a dynamically-significant role in clusters throughout their entire lifetimes. Here we review our latest understanding of BH populations in GCs and demonstrate that, through their dynamical interaction with their host cluster, BHs can naturally explain the distinction between core-collapsed and non-core-collapsed clusters through a process we call “black hole burning.”

Keywords

globular clustersblack holesdynamicsnumerical methodsgravitational waves
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. 357 - 366
Copyright
© International Astronomical Union 2020

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