Close encounters of black hole—star binaries with stellar-mass black holes

Author:

Ryu Taeho12ORCID,Valli Ruggero1ORCID,Pakmor Rüdiger1ORCID,Perna Rosalba34,de Mink Selma E15ORCID,Springel Volker1

Affiliation:

1. Max Planck Institute for Astrophysics , Karl-Schwarzschild-Str 1, 85748 Garching , Germany

2. Physics and Astronomy Department, Johns Hopkins University , 3400 N. Charles Street, Baltimore, MD 21218 , USA

3. Department of Physics and Astronomy, Stony Brook University , Stony Brook, NY 11794-3800 , USA

4. Center for Computational Astrophysics, Flatiron Institute , 162 5th Ave, New York, NY 10010 , USA

5. Anton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, 1098XH Amsterdam , the Netherlands

Abstract

ABSTRACT Dynamical interactions involving binaries play a crucial role in the evolution of star clusters and galaxies. We continue our investigation of the hydrodynamics of three-body encounters, focusing on binary black hole (BBH) formation, stellar disruption, and electromagnetic (EM) emission in dynamical interactions between a BH-star binary and a stellar-mass BH, using the moving-mesh hydrodynamics code AREPO. This type of encounters can be divided into two classes depending on whether the final outcome includes BBHs. This outcome is primarily determined by which two objects meet at the first closest approach. BBHs are more likely to form when the star and the incoming BH encounter first with an impact parameter smaller than the binary’s semimajor axis. In this case, the star is frequently disrupted. On the other hand, when the two BHs encounter first, frequent consequences are an orbit perturbation of the original binary or a binary member exchange. For the parameters chosen in this study, BBH formation, accompanied by stellar disruption, happens in roughly one out of four encounters. The close correlation between BBH formation and stellar disruption has possible implications for EM counterparts at the binary’s merger. The BH that disrupts the star is promptly surrounded by an optically and geometrically thick disc with accretion rates exceeding the Eddington limit. If the debris disc cools fast enough to become long-lived, EM counterparts can be produced at the time of the BBH merger.

Funder

Friedrich-Alexander-Universität Erlangen-Nürnberg

DFG

NSF

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 4 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Tidal disruption events from three-body scatterings and eccentricity pumping in the discs of active galactic nuclei;Monthly Notices of the Royal Astronomical Society;2024-05-13

2. Simulating the tidal disruption of stars by stellar-mass black holes using moving-mesh hydrodynamics;Astronomy & Astrophysics;2024-05

3. Tidal Disruption Encores;The Astrophysical Journal Letters;2024-04-01

4. Close encounters of star–black hole binaries with single stars;Monthly Notices of the Royal Astronomical Society;2023-10-10

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