scholarly journals Massive Black Holes in Star Clusters. I. Equal‐Mass Clusters

2004 ◽  
Vol 613 (2) ◽  
pp. 1133-1142 ◽  
Author(s):  
Holger Baumgardt ◽  
Junichiro Makino ◽  
Toshikazu Ebisuzaki
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Equal Mass ◽  
Massive Black Holes

scholarly journals Massive Black Holes in Star Clusters. II. Realistic Cluster Models

2004 ◽  
Vol 613 (2) ◽  
pp. 1143-1156 ◽  
Author(s):  
Holger Baumgardt ◽  
Junichiro Makino ◽  
Toshikazu Ebisuzaki
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Cluster Models ◽  
Massive Black Holes

scholarly journals THE COEVOLUTION OF NUCLEAR STAR CLUSTERS, MASSIVE BLACK HOLES, AND THEIR HOST GALAXIES

2015 ◽  
Vol 812 (1) ◽  
pp. 72 ◽  
Author(s):  
Fabio Antonini ◽  
Enrico Barausse ◽  
Joseph Silk
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Host Galaxies ◽  
Massive Black Holes

scholarly journals Defeating stochasticity: coalescence time-scales of massive black holes in galaxy mergers

2020 ◽  
Vol 497 (1) ◽  
pp. 739-746 ◽  
Author(s):  
Imran Nasim ◽  
Alessia Gualandris ◽  
Justin Read ◽  
Walter Dehnen ◽  
Maxime Delorme ◽  
...  
Keyword(s):  
Black Holes ◽  
Time Scale ◽  
Low Frequency ◽  
Primary Source ◽  
Equal Mass ◽  
Massive Black Hole ◽  
Low Frequencies ◽  
Detection Rates ◽  
Massive Black Holes ◽  
Numerical Resolution

ABSTRACT The coalescence of massive black hole binaries (BHBs) in galactic mergers is the primary source of gravitational waves (GWs) at low frequencies. Current estimates of GW detection rates for the Laser Interferometer Space Antenna and the Pulsar Timing Array vary by three orders of magnitude. To understand this variation, we simulate the merger of equal-mass, eccentric, galaxy pairs with central massive black holes and shallow inner density cusps. We model the formation and hardening of a central BHB using the fast multiple method as a force solver, which features a O(N) scaling with the number N of particles and obtains results equivalent to direct-summation simulations. At N ∼ 5 × 105, typical for contemporary studies, the eccentricity of the BHBs can vary significantly for different random realizations of the same initial condition, resulting in a substantial variation of the merger time-scale. This scatter owes to the stochasticity of stellar encounters with the BHB and decreases with increasing N. We estimate that N ∼ 107 within the stellar half-light radius suffices to reduce the scatter in the merger time-scale to ∼10 per cent. Our results suggest that at least some of the uncertainty in low-frequency GW rates owes to insufficient numerical resolution.

scholarly journals Black hole and nuclear cluster scaling relations: Mbh ∝ Mnc2.7±0.7

2014 ◽  
Vol 10 (S312) ◽  
pp. 269-273 ◽  
Author(s):  
Alister W. Graham
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Star Clusters ◽  
Compact Object ◽  
Scaling Relations ◽  
Black Hole Mass ◽  
Massive Black Holes ◽  
Mass Scaling ◽  
Nuclear Cluster ◽  
Evolutionary Growth

AbstractThere is a growing array of supermassive black hole and nuclear star cluster scaling relations with their host spheroid, including a bent (black hole mass)–(host spheroid mass) Mbh–Msph relation and a different (massive compact object mass)–(host spheroid velocity dispersion) Mmco–σ relations for black holes and nuclear star clusters. By combining the observed Mbh ∝ σ5.5 relation with the observed Mnc ∝ σ1.6–2.7 relation, we derive the expression Mbh ∝ Mnc2–3.4, which should hold until the nuclear star clusters are eventually destroyed in the larger core-Sérsic spheroids. This new mass scaling relation helps better quantify the rapid evolutionary growth of massive black holes in dense star clusters, and the relation is consistently recovered when coupling the observed Mnc ∝ Msph0.6–1.0 relation with the recently observed quadratic relation Mbh ∝ Msph2 for Sérsic spheroids.

scholarly journals Formation and Evolution of Massive Black Holes in Star Clusters

2005 ◽  
Vol 13 ◽  
pp. 350-353
Author(s):  
Holger Baumgardt ◽  
Junichiro Makino ◽  
Simon Portegies Zwart
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Initial Conditions ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Young Star ◽  
Cluster Center ◽  
Massive Black Hole ◽  
Massive Black Holes ◽  
Equilibrium Profile

AbstractWe present results of N-body simulations on the formation of massive black holes by run-away merging in young star clusters and the later dynamical evolution of star clusters containing massive black holes. We determine the initial conditions necessary for run-away merging to form a massive black hole and study the equilibrium profile that is established in the cluster center as a result of the interaction of stars with the central black hole. Our results show that star clusters which contain black holes have projected luminosity profiles that can be fitted by standard King models. The presence of massive black holes in (post-)core collapse clusters is therefore ruled out by our simulations.

scholarly journals Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse

2004 ◽  
Vol 604 (2) ◽  
pp. 632-652 ◽  
Author(s):  
M. Atakan Gurkan ◽  
Marc Freitag ◽  
Frederic A. Rasio
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Core Collapse ◽  
Massive Black Holes ◽  
Mass Segregation

scholarly journals Planetary systems in a star cluster II: intermediate-mass black holes and planetary systems

2020 ◽  
Vol 497 (3) ◽  
pp. 3623-3637
Author(s):  
Francesco Flammini Dotti ◽  
M B N Kouwenhoven ◽  
Qi Shu ◽  
Wei Hao ◽  
Rainer Spurzem
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Planetary Systems ◽  
Dynamical Evolution ◽  
Star Cluster ◽  
High Mass ◽  
Intermediate Mass ◽  
Massive Black Holes ◽  
Mass Segregation ◽  
Intermediate Mass Black Holes

ABSTRACT Most stars form in dense stellar environments. It is speculated that some dense star clusters may host intermediate-mass black holes (IMBHs), which may have formed from runaway collisions between high-mass stars, or from the mergers of less massive black holes. Here, we numerically explore the evolution of populations of planets in star clusters with an IMBH. We study the dynamical evolution of single-planet systems and free-floating planets, over a period of 100 Myr, in star clusters without an IMBH, and in clusters with a central IMBH of mass $100\, \mathrm{M}_\odot$ or $200\, \mathrm{M}_\odot$. In the central region ($r\lesssim 0.2$ pc), the IMBH’s tidal influence on planetary systems is typically 10 times stronger than the average neighbour star. For a star cluster with a $200\, \mathrm{M}_\odot$ IMBH, the region in which the IMBH’s influence is stronger within the virial radius (∼1 pc). The IMBH quenches mass segregation, and the stars in the core tend to move towards intermediate regions. The ejection rate of both stars and planets is higher when an IMBH is present. The rate at which planets are expelled from their host star rate is higher for clusters with higher IMBH masses, for t < 0.5trh, while remains mostly constant while the star cluster fills its Roche lobe, similar to a star cluster without an IMBH. The disruption rate of planetary systems is higher in initially denser clusters, and for wider planetary orbits, but this rate is substantially enhanced by the presence of a central IMBH.

scholarly journals Disolution of Star Clusters in Galaxies

1988 ◽  
Vol 126 ◽  
pp. 393-408 ◽  
Author(s):  
Roland Wielen
Keyword(s):  
Black Holes ◽  
Total Mass ◽  
Globular Clusters ◽  
Star Clusters ◽  
Major Constituent ◽  
Dissolution Time ◽  
Massive Black Holes

We present a procedure which allows to predict the dissolution times of star clusters in a simple way. The dissolution time of a cluster depends mainly on its total mass, its median radius and its galactic environment (galactic tidal field and passing massive objects). As an example, we discuss the lifetimes of LMC clusters. Finally, we show that massive black holes, which have been proposed as the major constituent of the dark coronae of galaxies, are very effective in destroying globular clusters.

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