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 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 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 The Clustering Dynamics of Primordial Black Boles in N-Body Simulations

Universe ◽  
2021 ◽  
Vol 7 (1) ◽  
pp. 18
Author(s):  
Manuel Trashorras ◽  
Juan García-Bellido ◽  
Savvas Nesseris
Keyword(s):  
Black Holes ◽  
Binary Systems ◽  
Orbital Parameter ◽  
Galactic Halos ◽  
Massive Black Holes ◽  
Close Encounters ◽  
Mass Ratios ◽  
History Of ◽  
Mass Segregation ◽  
Rate Of Evaporation

We explore the possibility that Dark Matter (DM) may be explained by a nonuniform background of approximately stellar mass clusters of Primordial Black Holes (PBHs) by simulating the evolution from recombination to the present with over 5000 realisations using a Newtonian N-body code. We compute the cluster rate of evaporation and extract the binary and merged sub-populations along with their parent and merger tree histories, lifetimes and formation rates, the dynamical and orbital parameter profiles, the degree of mass segregation and dynamical friction and power spectrum of close encounters. Overall, we find that PBHs can constitute a viable DM candidate, and that their clustering presents a rich phenomenology throughout the history of the Universe. We show that binary systems constitute about 9.5% of all PBHs at present, with mass ratios of q¯B=0.154, and total masses of m¯T,B=303M⊙. Merged PBHs are rare, about 0.0023% of all PBHs at present, with mass ratios of q¯B=0.965 with total and chirp masses of m¯T,B=1670M⊙ and m¯c,M=642M⊙, respectively. We find that cluster puffing up and evaporation leads to bubbles of these PBHs of order 1 kpc containing at present times about 36% of objects and mass, with one-hundred pc-sized cores. We also find that these PBH sub-haloes are distributed in wider PBH haloes of order hundreds of kpc, containing about 63% of objects and mass, coinciding with the sizes of galactic halos. We find at last high rates of close encounters of massive Black Holes (M∼1000M⊙), with ΓS=(1.2+5.9−0.9)×107yr−1Gpc−3 and mergers with ΓM=1337±41yr−1Gpc−3.

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.

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