scholarly journals Inspiral, merger, and ring-down of equal-mass black-hole binaries

2007 ◽  
Vol 75 (12) ◽  
Author(s):  
Alessandra Buonanno ◽  
Gregory B. Cook ◽  
Frans Pretorius
Keyword(s):  
Black Hole ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Stellar hardening of massive black hole binaries: the impact of the host rotation

2021 ◽  
Vol 508 (1) ◽  
pp. 1533-1542
Author(s):  
Ludovica Varisco ◽  
Elisa Bortolas ◽  
Massimo Dotti ◽  
Alberto Sesana
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Equal Mass ◽  
Stellar Systems ◽  
Massive Black Hole ◽  
Loss Cone ◽  
Black Hole Binaries ◽  
Influence Radius ◽  
Three Body ◽  
The Impact

ABSTRACT Massive black hole binaries (MBHBs) with masses of ∼104 to $\sim 10^{10} \, \mathrm{M}_{\odot {}}$ are one of the main targets for currently operating and forthcoming space-borne gravitational wave observatories. In this paper, we explore the effect of the stellar host rotation on the bound binary hardening efficiency, driven by three-body stellar interactions. As seen in previous studies, we find that the centre of mass (CoM) of a prograde MBHB embedded in a rotating environment starts moving on a nearly circular orbit about the centre of the system shortly after the MBHB binding. In our runs, the oscillation radius is ≈ 0.25 (≈ 0.1) times the binary influence radius for equal mass MBHBs (MBHBs with mass ratio 1:4). Conversely, retrograde binaries remain anchored about the centre of the host. The binary shrinking rate is twice as fast when the binary CoM exhibits a net orbital motion, owing to a more efficient loss cone repopulation even in our spherical stellar systems. We develop a model that captures the CoM oscillations of prograde binaries; we argue that the CoM angular momentum gain per time unit scales with the internal binary angular momentum, so that most of the displacement is induced by stellar interactions occurring around the time of MBHB binding, while the subsequent angular momentum enhancement gets eventually quashed by the effect of dynamical friction. The effect of the background rotation on the MBHB evolution may be relevant for LISA sources, that are expected to form in significantly rotating stellar systems.

scholarly journals Numerical simulations of neutron star-black hole binaries in the near-equal-mass regime

2019 ◽  
Vol 99 (10) ◽  
Author(s):  
F. Foucart ◽  
M. D. Duez ◽  
L. E. Kidder ◽  
S. M. Nissanke ◽  
H. P. Pfeiffer ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Numerical Simulations ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Momentum flow in black-hole binaries. II. Numerical simulations of equal-mass, head-on mergers with antiparallel spins

2010 ◽  
Vol 82 (6) ◽  
Author(s):  
Geoffrey Lovelace ◽  
Yanbei Chen ◽  
Michael Cohen ◽  
Jeffrey D. Kaplan ◽  
Drew Keppel ◽  
...  
Keyword(s):  
Black Hole ◽  
Numerical Simulations ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Spin Diagrams for Equal‐Mass Black Hole Binaries with Aligned Spins

2008 ◽  
Vol 679 (2) ◽  
pp. 1422-1426 ◽  
Author(s):  
Luciano Rezzolla ◽  
Ernst Nils Dorband ◽  
Christian Reisswig ◽  
Peter Diener ◽  
Denis Pollney ◽  
...  
Keyword(s):  
Black Hole ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Faithful effective-one-body waveforms of equal-mass coalescing black-hole binaries

2008 ◽  
Vol 77 (8) ◽  
Author(s):  
Thibault Damour ◽  
Alessandro Nagar ◽  
Ernst Nils Dorband ◽  
Denis Pollney ◽  
Luciano Rezzolla
Keyword(s):  
Black Hole ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Gravitational-wave detectability of equal-mass black-hole binaries with aligned spins

2009 ◽  
Vol 80 (12) ◽  
Author(s):  
Christian Reisswig ◽  
Sascha Husa ◽  
Luciano Rezzolla ◽  
Ernst Nils Dorband ◽  
Denis Pollney ◽  
...  
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Equal Mass ◽  
Black Hole Binaries

scholarly journals Formation of counter-rotating and highly eccentric massive black hole binaries in galaxy mergers

2021 ◽  
Vol 503 (1) ◽  
pp. 498-510
Author(s):  
Imran Tariq Nasim ◽  
Cristobal Petrovich ◽  
Adam Nasim ◽  
Fani Dosopoulou ◽  
Fabio Antonini
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Dynamical Evolution ◽  
Orbital Plane ◽  
Equal Mass ◽  
Galaxy Mergers ◽  
High Eccentricity ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Binary Evolution

ABSTRACT Supermassive black hole (SMBH) binaries represent the main target for missions such as the Laser Interferometer Space Antenna and Pulsar Timing Arrays. The understanding of their dynamical evolution prior to coalescence is therefore crucial to improving detection strategies and for the astrophysical interpretation of the gravitational wave data. In this paper, we use high-resolution N-body simulations to model the merger of two equal-mass galaxies hosting a central SMBH. In our models, all binaries are initially prograde with respect to the galaxy sense of rotation. But, binaries that form with a high eccentricity, e ≳ 0.7, quickly reverse their sense of rotation and become almost perfectly retrograde at the moment of binary formation. The evolution of these binaries proceeds towards larger eccentricities, as expected for a binary hardening in a counter-rotating stellar distribution. Binaries that form with lower eccentricities remain prograde and at comparatively low eccentricities. We study the origin of the orbital flip by using an analytical model that describes the early stages of binary evolution. This model indicates that the orbital plane flip is due to the torque from the triaxial background mass distribution that naturally arises from the galactic merger process. Our results imply the existence of a population of SMBH binaries with a high eccentricity and could have significant implications for the detection of the gravitational wave signal emitted by these systems.

scholarly journals On the equal-mass limit of precessing black-hole binaries

2017 ◽  
Vol 34 (6) ◽  
pp. 064004 ◽  
Author(s):  
Davide Gerosa ◽  
Ulrich Sperhake ◽  
Jakub Vošmera
Keyword(s):  
Black Hole ◽  
Equal Mass ◽  
Mass Limit ◽  
Black Hole Binaries

scholarly journals Formation of discs around super-massive black hole binaries

2014 ◽  
Vol 10 (S312) ◽  
pp. 48-51
Author(s):  
Felipe G. Goicovic ◽  
Jorge Cuadra ◽  
Alberto Sesana
Keyword(s):  
Black Hole ◽  
Molecular Clouds ◽  
Equal Mass ◽  
Massive Black Hole ◽  
Black Hole Binaries ◽  
Supermassive Black Hole ◽  
First Results

AbstractWe model numerically the evolution of 104M⊙ turbulent molecular clouds in near-radial infall onto 106M⊙, equal-mass supermassive black hole binaries, using a modified version of the SPH code gadget-3. We investigate the different gas structures formed depending on the relative inclination between the binary and the cloud orbits. Our first results indicate that an aligned orbit produces mini-discs around each black hole, almost aligned with the binary; a perpendicular orbit produces misaligned mini-discs; and a counter-aligned orbit produces a circumbinary, counter-rotating ring.

scholarly journals Evolution of supermassive black hole binaries in gaseous environments

2015 ◽  
Vol 11 (A29B) ◽  
pp. 314-316
Author(s):  
Giuseppe Lodato
Keyword(s):  
Black Hole ◽  
Mass Flow ◽  
Dynamical Evolution ◽  
Equal Mass ◽  
Accretion Discs ◽  
Tidal Torque ◽  
Black Hole Binaries ◽  
Supermassive Black Hole ◽  
Binary Component ◽  
Flow Through

AbstractIn this contribution, I discuss some aspects of the dynamical evolution of supermassive black hole binaries and their accretion discs. Firstly, I discuss the issue of alignment of the spins of the two binary component, which has important implications for the shape of the gravitational wave emitted at merger and for the possibility of a strong recoil of the remnant black hole. Even under the favourable assumption that mass flow through the gap is not inhibited by tidal torque, we demonstrate that differential accretion onto the two components of the systems results in a very different spin evolution of the two black holes. Secondly, I revisit the issue of how much mass can flow within the cavity carved in the disc by an equal mass binary. Recent simulations have shown that the tidal torque of the binary is generally not sufficient to prevent accretion onto the binary component. Here, I demonstrate that such results are heavily dependent on the disc thickness. While for H/R ~ 0.1 (the value adopted in most simulations to date), we reproduce the previous results, we show that as H/R is decreased to ~ 0.01, mass flow through the gap is essentially shut off almost completely. Thirdly, I show numerical simulations of the process of gas squeezing during the merger proper, demonstrating that most of the disc mass is accreted producing a super-Eddington flare.

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