scholarly journals Features of globular cluster’s dynamics with an intermediate-mass black hole

2018 ◽  
Vol 27 (1) ◽  
pp. 1-6 ◽  
Author(s):  
Marina V. Ryabova ◽  
Alena S. Gorban ◽  
Yuri A. Shchekinov ◽  
Evgenii O. Vasiliev
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Globular Cluster ◽  
Binary Stars ◽  
Stellar Mass ◽  
Core Collapse ◽  
Intermediate Mass

Abstract In this paper, we address the question of how a central intermediate-mass black hole (IMBH) in a globular cluster (GC) affects dynamics, core collapse, and formation of the binary population. It is shown that the central IMBH forms a binary system that affects dynamics of stars in the cluster significantly. The presence of an intermediate-mass black hole with mass ≥ 1.0-1.7%of the total stellar mass in the cluster inhibits the formation of binary stars population.

scholarly journals Dynamical Evolution of Star Clusters with Intermediate Mass Black Holes and Primordial Binaries

2007 ◽  
Vol 3 (S246) ◽  
pp. 256-260
Author(s):  
Michele Trenti
Keyword(s):  
Black Hole ◽  
Binary Stars ◽  
Initial Conditions ◽  
Relaxation Times ◽  
Star Clusters ◽  
Dynamical Evolution ◽  
Star Cluster ◽  
Core Collapse ◽  
Large Set ◽  
Intermediate Mass

AbstractThe evolution of a star cluster is strongly influenced by the presence of primordial binaries and of a central black hole, as dynamical interactions within the core prevents a deep core collapse under these conditions. We present the results from a large set of direct N-body simulations of star clusters that include an intermediate mass black hole, single and binary stars. We highlight the structural and dynamical differences for the various cases showing in particular that on a timescale of a few relaxation times the density profile of the star cluster does no longer depend on the details of the initial conditions but only on the efficiency of the energy generation due to gravitational encounters at the center of the system.

scholarly journals RBS 1032: a dwarf-nucleated spheroidal galaxy with an intermediate-mass black hole hosted in a globular cluster

2006 ◽  
Vol 371 (4) ◽  
pp. 1587-1593 ◽  
Author(s):  
K. K. Ghosh ◽  
V. Suleymanov ◽  
I. Bikmaev ◽  
S. Shimansky ◽  
N. Sakhibullin
Keyword(s):  
Black Hole ◽  
Globular Cluster ◽  
Intermediate Mass

scholarly journals No evidence for intermediate-mass black holes in the globular clusters ω Cen and NGC 6624

2019 ◽  
Vol 488 (4) ◽  
pp. 5340-5351 ◽  
Author(s):  
H Baumgardt ◽  
C He ◽  
S M Sweet ◽  
M Drinkwater ◽  
A Sollima ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Globular Clusters ◽  
Surface Brightness ◽  
Velocity Dispersion ◽  
Stellar Mass ◽  
Main Sequence Stars ◽  
Intermediate Mass ◽  
Measured Velocity ◽  
Large Grid

ABSTRACT We compare the results of a large grid of N-body simulations with the surface brightness and velocity dispersion profiles of the globular clusters ω Cen and NGC 6624. Our models include clusters with varying stellar-mass black hole retention fractions and varying masses of a central intermediate-mass black hole (IMBH). We find that an $\sim 45\, 000$ M⊙ IMBH, whose presence has been suggested based on the measured velocity dispersion profile of ω Cen, predicts the existence of about 20 fast-moving, m > 0.5 M⊙, main-sequence stars with a (1D) velocity v > 60 km s−1 in the central 20 arcsec of ω Cen. However, no such star is present in the HST/ACS proper motion catalogue of Bellini et al. (2017), strongly ruling out the presence of a massive IMBH in the core of ω Cen. Instead, we find that all available data can be fitted by a model that contains 4.6 per cent of the mass of ω Cen in a centrally concentrated cluster of stellar-mass black holes. We show that this mass fraction in stellar-mass BHs is compatible with the predictions of stellar evolution models of massive stars. We also compare our grid of N-body simulations with NGC 6624, a cluster recently claimed to harbour a 20 000 M⊙ black hole based on timing observations of millisecond pulsars. However, we find that models with MIMBH > 1000 M⊙ IMBHs are incompatible with the observed velocity dispersion and surface brightness profile of NGC 6624, ruling out the presence of a massive IMBH in this cluster. Models without an IMBH provide again an excellent fit to NGC 6624.

scholarly journals Explosion of very massive stars and the origin of intermediate mass black holes

2006 ◽  
Vol 2 (S238) ◽  
pp. 241-246
Author(s):  
Sachiko Tsuruta ◽  
Takuya Ohkubo ◽  
Hideyuki Umeda ◽  
Keiichi Maeda ◽  
Ken'ichi Nomoto ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Massive Stars ◽  
Core Collapse ◽  
Clusters Of Galaxies ◽  
Intermediate Mass ◽  
Black Hole Masses ◽  
Better Than ◽  
Intermediate Mass Black Holes ◽  
Population Iii

AbstractWe calculate evolution, collapse, explosion, and nucleosynthesis of Population III very massive stars with 500 M⊙ and 1000 M⊙. It was found that both 500 M⊙ and 1000 M⊙ models enter the region of pair-instability but continue to undergo core collapse to black holes. For moderately aspherical explosions, the patterns of nucleosynthesis match the observational data of intergalactic and intercluster medium and hot gases in M82, better than models involving hypernovae and pair instability supernovae.Our results suggest that explosions of Population III core-collapse very massive stars contribute significantly to the chemical evolution of gases in clusters of galaxies. The final black hole masses are about 500 M⊙ for our most massive 1000 M⊙ models. This result may support the view that Population III very massive stars are responsible for the origin of intermediate mass black holes which were recently reported to be discovered.

scholarly journals VVV SURVEY OBSERVATIONS OF A MICROLENSING STELLAR MASS BLACK HOLE CANDIDATE IN THE FIELD OF THE GLOBULAR CLUSTER NGC 6553

2015 ◽  
Vol 810 (2) ◽  
pp. L20 ◽  
Author(s):  
D. Minniti ◽  
R. Contreras Ramos ◽  
J. Alonso-García ◽  
T. Anguita ◽  
M. Catelan ◽  
...  
Keyword(s):  
Black Hole ◽  
Globular Cluster ◽  
Stellar Mass ◽  
Black Hole Candidate

scholarly journals Radio Emission from the Intermediate-Mass Black Hole in the Globular Cluster G1

2007 ◽  
Vol 661 (2) ◽  
pp. L151-L154 ◽  
Author(s):  
James S. Ulvestad ◽  
Jenny E. Greene ◽  
Luis C. Ho
Keyword(s):  
Black Hole ◽  
Radio Emission ◽  
Globular Cluster ◽  
Intermediate Mass

scholarly journals Evidence for an intermediate-mass black hole in the globular cluster NGC 6624

2017 ◽  
Vol 468 (2) ◽  
pp. 2114-2127 ◽  
Author(s):  
B. B. P. Perera ◽  
B. W. Stappers ◽  
A. G. Lyne ◽  
C. G. Bassa ◽  
I. Cognard ◽  
...  
Keyword(s):  
Black Hole ◽  
Globular Cluster ◽  
Intermediate Mass

scholarly journals POPULATION OF BLACK HOLES IN THE MILKY WAY AND IN THE MAGELLANIC CLOUDS

2013 ◽  
Vol 53 (A) ◽  
pp. 665-670
Author(s):  
Janusz Ziółkowski
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Milky Way ◽  
Stellar Mass ◽  
Magellanic Clouds ◽  
Intermediate Mass ◽  
Different Types ◽  
The Galaxy

In this review, I will briefly discuss the different types of black hole (BH) populations (supermassive, intermediate mass and stellar mass BHs) both in the Galaxy and in the Magellanic Clouds and compare them with each other.

scholarly journals mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes

2020 ◽  
Vol 498 (3) ◽  
pp. 4287-4294
Author(s):  
Jongsuk Hong ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Arkadiusz Hypki ◽  
Suk-Jin Yoon
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Globular Clusters ◽  
Stellar Mass ◽  
Intermediate Mass ◽  
Binary Black Holes ◽  
Black Hole Binaries ◽  
Binary Black Hole ◽  
Intermediate Mass Black Holes

ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.

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