scholarly journals Merger rate of black hole binaries from globular clusters: Theoretical error bars and comparison to gravitational wave data from GWTC-2

2020 ◽  
Vol 102 (12) ◽  
Author(s):  
Fabio Antonini ◽  
Mark Gieles
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Globular Clusters ◽  
Black Hole Binaries ◽  
Wave Data ◽  
Theoretical Error ◽  
Error Bars ◽  
Merger Rate

scholarly journals A Dynamical Gravitational Wave Source in a Dense Cluster

2016 ◽  
Vol 33 ◽  
Author(s):  
Jarrod R. Hurley ◽  
Anna C. Sippel ◽  
Christopher A. Tout ◽  
Sverre J. Aarseth
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Globular Clusters ◽  
Binary Systems ◽  
Star Cluster ◽  
High Density ◽  
Wave Source ◽  
Black Hole Binaries ◽  
Dense Cluster

AbstractMaking use of a new N-body model to describe the evolution of a moderate-size globular cluster, we investigate the characteristics of the population of black holes within such a cluster. This model reaches core-collapse and achieves a peak central density typical of the dense globular clusters of the Milky Way. Within this high-density environment, we see direct confirmation of the merging of two stellar remnant black holes in a dynamically formed binary, a gravitational wave source. We describe how the formation, evolution, and ultimate ejection/destruction of binary systems containing black holes impacts the evolution of the cluster core. Also, through comparison with previous models of lower density, we show that the period distribution of black hole binaries formed through dynamical interactions in this high-density model favours the production of gravitational wave sources. We confirm that the number of black holes remaining in a star cluster at late times and the characteristics of the binary black hole population depend on the nature of the star cluster, critically on the number density of stars and by extension the relaxation timescale.

scholarly journals Dynamically formed black hole binaries: In-cluster versus ejected mergers

2020 ◽  
Vol 37 ◽  
Author(s):  
O. Anagnostou ◽  
M. Trenti ◽  
A. Melatos
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Gravitational Radiation ◽  
Globular Clusters ◽  
Initial Conditions ◽  
Ratio Distribution ◽  
Black Hole Binaries ◽  
Tidal Interactions ◽  
Age Of The Universe ◽  
Cluster Mergers

Abstract The growing number of black hole binary (BHB) mergers detected by the Laser Interferometer Gravitational-Wave Observatory have the potential to enable an unprecedented characterisation of the physical processes and astrophysical conditions that govern the formation of compact binaries. In this paper, we focus on investigating the dynamical formation of BHBs in dense star clusters through a state-of-the-art set of 58 direct N-body simulations with N $\leqslant200\,000$ particles which include stellar evolution, gravitational braking, orbital decay through gravitational radiation, and galactic tidal interactions. The simulations encompass a range of initial conditions representing typical young globular clusters, including the presence of primordial binaries. The systems are simulated for $\sim 12$ Gyr. The dataset yields 117 BHB gravitational wave (GW) events, with 97 binaries merging within their host cluster and 20 merging after having been ejected. Only 8% of all ejected BHBs merge within the age of the Universe. Systems in this merging subset tend to have smaller separations and larger eccentricities, as this combination of parameters results in greater emission of gravitational radiation. We confirm known trends from Monte Carlo simulations, such as the anti-correlation between the mass of the binary and age of the cluster. In addition, we highlight for the first time a difference at low values of the mass ratio distribution between in-cluster and ejected mergers. However, the results depend on assumptions on the strength of GW recoils, thus in-cluster mergers cannot be ruled out at a significant level of confidence. A more substantial catalogue of BHB mergers and a more extensive library of N-body simulations are needed to constrain the origin of the observed events.

Gravitational waves from neutron star binaries

2017 ◽  
Vol 26 (01n02) ◽  
pp. 1740015 ◽  
Author(s):  
Chang-Hwan Lee
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Future Prospect ◽  
Black Hole Binaries ◽  
Wave Detection ◽  
Low Mass ◽  
Merger Rate

With H. A. Bethe, G. E. Brown worked on the merger rate of neutron star binaries for the gravitational wave detection. Their prediction has to be modified significantly due to the observations of [Formula: see text] neutron stars and the detection of gravitational waves. There still, however, remains a possibility that neutron star-low mass black hole binaries are significant sources of gravitational waves for the ground-based detectors. In this paper, I review the evolution of neutron star binaries with super-Eddington accretion and discuss the future prospect.

scholarly journals Low significance of evidence for black hole echoes in gravitational wave data

2018 ◽  
Vol 97 (12) ◽  
Author(s):  
Julian Westerweck ◽  
Alex B. Nielsen ◽  
Ofek Fischer-Birnholtz ◽  
Miriam Cabero ◽  
Collin Capano ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Wave Data

scholarly journals The local nanohertz gravitational-wave landscape from supermassive black hole binaries

2017 ◽  
Vol 1 (12) ◽  
pp. 886-892 ◽  
Author(s):  
Chiara M. F. Mingarelli ◽  
T. Joseph W. Lazio ◽  
Alberto Sesana ◽  
Jenny E. Greene ◽  
Justin A. Ellis ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Black Hole Binaries ◽  
Supermassive Black Hole

scholarly journals Population synthesis of black hole binary mergers from star clusters

2020 ◽  
Vol 492 (2) ◽  
pp. 2936-2954 ◽  
Author(s):  
Fabio Antonini ◽  
Mark Gieles
Keyword(s):  
Black Hole ◽  
Globular Clusters ◽  
Initial Conditions ◽  
Star Clusters ◽  
Population Synthesis ◽  
Wide Range ◽  
Binary Mergers ◽  
Cluster Properties ◽  
Black Hole Binary ◽  
Merger Rate

ABSTRACT Black hole (BH) binary mergers formed through dynamical interactions in dense star clusters are believed to be one of the main sources of gravitational waves (GWs) for Advanced LIGO and Virgo. Here, we present a fast numerical method for simulating the evolution of star clusters with BHs, including a model for the dynamical formation and merger of BH binaries. Our method is based on Hénon’s principle of balanced evolution, according to which the flow of energy within a cluster must be balanced by the energy production inside its core. Because the heat production in the core is powered by the BHs, one can then link the evolution of the cluster to the evolution of its BH population. This allows us to construct evolutionary tracks of the cluster properties including its BH population and its effect on the cluster and, at the same time, determine the merger rate of BH binaries as well as their eccentricity distributions. The model is publicly available and includes the effects of a BH mass spectrum, mass-loss due to stellar evolution, the ejection of BHs due to natal and dynamical kicks, and relativistic corrections during binary–single encounters. We validate our method using direct N-body simulations, and find it to be in excellent agreement with results from recent Monte Carlo models of globular clusters. This establishes our new method as a robust tool for the study of BH dynamics in star clusters and the modelling of GW sources produced in these systems. Finally, we compute the rate and eccentricity distributions of merging BH binaries for a wide range of cluster initial conditions, spanning more than two orders of magnitude in mass and radius.

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