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MOCCA-SURVEY data base II – Properties of intermediate mass black holes escaping from star clusters

Maliszewski, Konrad ; Giersz, Mirek ; Gondek-Rosinska, Dorota ; Askar, Abbas LU orcid and Hypki, Arkadiusz (2022) In Monthly Notices of the Royal Astronomical Society 514(4). p.5879-5889
Abstract
In this work, we investigate properties of intermediate-mass black holes
(IMBHs) that escape from star clusters due to dynamical interactions.
The studied models were simulated as part of the preliminary second
survey carried out using the MOCCA code (MOCCA-SURVEY Database II),
which is based on the Monte Carlo N-body method and does not
include gravitational wave recoil kick prescriptions of the binary black
hole merger product. We have found that IMBHs are more likely to be
formed and ejected in models where both initial central density and
central escape velocities have high values. Most of our studied objects
escape in a binary with another black hole (BH) as their companion and... (More)
In this work, we investigate properties of intermediate-mass black holes
(IMBHs) that escape from star clusters due to dynamical interactions.
The studied models were simulated as part of the preliminary second
survey carried out using the MOCCA code (MOCCA-SURVEY Database II),
which is based on the Monte Carlo N-body method and does not
include gravitational wave recoil kick prescriptions of the binary black
hole merger product. We have found that IMBHs are more likely to be
formed and ejected in models where both initial central density and
central escape velocities have high values. Most of our studied objects
escape in a binary with another black hole (BH) as their companion and
have masses between 100 and 140 M⊙⁠.
Escaping IMBHs tend to build-up mass most effectively through repeated
mergers in a binary with BHs due to gravitational wave emission.
Binaries play a key role in their ejection from the system as they allow
these massive objects to gather energy needed for escape. The binaries
in which IMBHs escape tend to have very high binding energy at the time
of escape and the last interaction is strong but does not involve a
massive intruder. These IMBHs gain energy needed to escape the cluster
gradually in successive dynamical interactions. We present specific
examples of the history of IMBH formation and escape from star cluster
models. We also discuss the observational implications of our findings
as well as the potential influence of the gravitational wave recoil
kicks on the process. (Less)
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author
; ; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
galaxies: star clusters: general, methods: numerical
in
Monthly Notices of the Royal Astronomical Society
volume
514
issue
4
pages
5879 - 5889
publisher
Oxford University Press
external identifiers
  • scopus:85135153099
ISSN
1365-2966
DOI
10.1093/mnras/stac1728
language
English
LU publication?
yes
id
5b018ef9-f2e4-4cb5-9ad6-8829fd8c3afd
date added to LUP
2022-07-18 14:20:17
date last changed
2024-04-18 09:31:05
@article{5b018ef9-f2e4-4cb5-9ad6-8829fd8c3afd,
  abstract     = {{In this work, we investigate properties of intermediate-mass black holes<br>
 (IMBHs) that escape from star clusters due to dynamical interactions. <br>
The studied models were simulated as part of the preliminary second <br>
survey carried out using the MOCCA code (MOCCA-SURVEY Database II), <br>
which is based on the Monte Carlo <em>N</em>-body method and does not <br>
include gravitational wave recoil kick prescriptions of the binary black<br>
 hole merger product. We have found that IMBHs are more likely to be <br>
formed and ejected in models where both initial central density and <br>
central escape velocities have high values. Most of our studied objects <br>
escape in a binary with another black hole (BH) as their companion and <br>
have masses between 100 and 140 M⊙⁠.<br>
 Escaping IMBHs tend to build-up mass most effectively through repeated <br>
mergers in a binary with BHs due to gravitational wave emission. <br>
Binaries play a key role in their ejection from the system as they allow<br>
 these massive objects to gather energy needed for escape. The binaries <br>
in which IMBHs escape tend to have very high binding energy at the time <br>
of escape and the last interaction is strong but does not involve a <br>
massive intruder. These IMBHs gain energy needed to escape the cluster <br>
gradually in successive dynamical interactions. We present specific <br>
examples of the history of IMBH formation and escape from star cluster <br>
models. We also discuss the observational implications of our findings <br>
as well as the potential influence of the gravitational wave recoil <br>
kicks on the process.}},
  author       = {{Maliszewski, Konrad and Giersz, Mirek and Gondek-Rosinska, Dorota and Askar, Abbas and Hypki, Arkadiusz}},
  issn         = {{1365-2966}},
  keywords     = {{galaxies: star clusters: general; methods: numerical}},
  language     = {{eng}},
  month        = {{07}},
  number       = {{4}},
  pages        = {{5879--5889}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{MOCCA-SURVEY data base II – Properties of intermediate mass black holes escaping from star clusters}},
  url          = {{http://dx.doi.org/10.1093/mnras/stac1728}},
  doi          = {{10.1093/mnras/stac1728}},
  volume       = {{514}},
  year         = {{2022}},
}