scholarly journals Energy and angular momentum radiated for non-head-on binary black hole collisions

2002 ◽  
Vol 66 (10) ◽  
Author(s):  
Osvaldo Moreschi ◽  
Alejandro Perez ◽  
Luis Lehner
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Binary Black Hole

scholarly journals Decline of the Current Quadrupole Moment during the Merger Phase of Binary Black Hole Coalescence

Universe ◽  
2019 ◽  
Vol 6 (1) ◽  
pp. 3
Author(s):  
Fan Zhang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Quadrupole Moment ◽  
Total Angular Momentum ◽  
Quasinormal Modes ◽  
Binary Black Hole ◽  
Mass Quadrupole

Utilizing the tools of tendex and vortex, we study the highly dynamic plunge and merger phases of several π -symmetric binary black hole coalescences. In particular, we observe a decline of the strength of the current quadrupole moment compared to that of the mass quadrupole moment during the merger phase, contrary to a naive estimate according to the dependence of these moments on the separation between the black holes. We further show that this decline of the current quadrupole moment is achieved through the remnants of the two individual spins becoming nearly aligned or anti-aligned with the total angular momentum. We also speculate on the ability to achieve a consistency between the electric and magnetic parity quasinormal modes.

scholarly journals Coalescence of Kerr Black Holes—Binary Systems from GW150914 to GW170814

Entropy ◽  
2019 ◽  
Vol 21 (10) ◽  
pp. 1017
Author(s):  
Bogeun Gwak
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Gravitational Wave ◽  
Orbital Angular Momentum ◽  
Binary Systems ◽  
Analytical Form ◽  
Angular Momenta ◽  
Binary Black Hole ◽  
Kerr Black Holes

We investigate the energy of the gravitational wave from a binary black hole merger by the coalescence of two Kerr black holes with an orbital angular momentum. The coalescence is constructed to be consistent with particle absorption in the limit in which the primary black hole is sufficiently large compared with the secondary black hole. In this limit, we analytically obtain an effective gravitational spin–orbit interaction dependent on the alignments of the angular momenta. Then, binary systems with various parameters including equal masses are numerically analyzed. According to the numerical analysis, the energy of the gravitational wave still depends on the effective interactions, as expected from the analytical form. In particular, we ensure that the final black hole obtains a large portion of its spin angular momentum from the orbital angular momentum of the initial binary black hole. To estimate the angular momentum released by the gravitational wave in the actual binary black hole, we apply our results to observations at the Laser Interferometer Gravitational-Wave Observatory: GW150914, GW151226, GW170104, GW170608 and GW170814.

Properties of dynamical space-times

2018 ◽  
Author(s):  
Michele Maggiore
Keyword(s):  
General Relativity ◽  
Black Hole ◽  
Angular Momentum ◽  
Gravitational Radiation ◽  
Hamiltonian Formulation ◽  
Black Hole Mass ◽  
Adm Mass ◽  
Binary Black Hole

An introduction to advanced tools of General Relativity, later used in the study of binary black-hole coalescences. Hamiltonian formulation of General Relativity, ADM mass and angular momentum, irreducible black-hole mass, Newman-Penrose scalars and gravitational radiation.

scholarly journals Gravitational and electromagnetic radiation from binary black holes with electric and magnetic charges: elliptical orbits on a cone

2021 ◽  
Vol 81 (11) ◽  
Author(s):  
Lang Liu ◽  
Øyvind Christiansen ◽  
Wen-Hong Ruan ◽  
Zong-Kuan Guo ◽  
Rong-Gen Cai ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Gravitational Waves ◽  
Emission Rates ◽  
Total Emission ◽  
Binary Black Holes ◽  
Binary Black Hole ◽  
Elliptical Orbits ◽  
Electromagnetic Radiations

AbstractExtending the electromagnetic and gravitational radiations from binary black holes with electric and magnetic charges in circular orbits in Liu et al. (Phys. Rev. D 102:103520, 2020), we calculate the total emission rates of energy and angular momentum due to gravitational and electromagnetic radiations from dyonic binary black holes in precessing elliptical orbits. It is shown that the emission rates of energy and angular momentum due to gravitational and electromagnetic radiations have the same dependence on the conic angle for different orbits. Moreover, we obtain the evolutions of orbits and find that a circular orbit remains circular while an elliptic orbit becomes quasi-circular due to electromagnetic and gravitational radiations. Using the evolution of orbits, we derive the waveform models for dyonic binary black hole inspirals and show the amplitudes of the gravitational waves for dyonic binary black hole inspirals differ from those for Schwarzschild binary black hole inspirals, which can be used to test electric and magnetic charges of black holes.

SPIN EXPANSION FOR HEAD-ON COLLISION OF TWO BLACK HOLES

2011 ◽  
Vol 20 (01) ◽  
pp. 43-57 ◽  
Author(s):  
ZHOUJIAN CAO ◽  
CHENZHOU LIU
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Orbital Angular Momentum ◽  
New Method ◽  
Initial State ◽  
Final State ◽  
The Third ◽  
Binary Black Hole ◽  
Expansion Technique

The spin expansion technique proposed in [L. Boyel, M. Kesden and S. Nissanke, Phys. Rev. Lett.100 (2008) 151101] is very powerful to analyze the relation between the initial state of binary black hole and the final state of the merged black hole. But this technique needs orbital angular momentum to determine the third direction of a triad. Without this triad we cannot get the decomposed components of the involved quantities, and the spin expansion breaks down. The head-on collision of two black holes, whose orbital angular momentum vanishes, falls into this case. In this paper we propose a new method to construct a triad for spin expansion technique. With this new method, we get the same set of equations as in the above-mentioned paper. Furthermore, we use numerical simulations to illustrate the validity of our new method for the head-on collision of two black holes.

scholarly journals Symmetry Breaking in Dynamical Encounters in the Disks of Active Galactic Nuclei

2021 ◽  
Vol 923 (2) ◽  
pp. L23
Author(s):  
Yi-Han Wang ◽  
Barry McKernan ◽  
Saavik Ford ◽  
Rosalba Perna ◽  
Nathan W. C. Leigh ◽  
...  
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Active Galactic Nuclei ◽  
Numerical Experiments ◽  
Semimajor Axis ◽  
Galactic Nuclei ◽  
High Accuracy ◽  
Broken Symmetry ◽  
Asymmetric Distribution ◽  
Binary Black Hole

Abstract The disks of active galactic nuclei (AGNs) may be important sites of binary black hole (BBH) mergers. Here we show via numerical experiments with the high-accuracy, high-precision code SpaceHub that broken symmetry in dynamical encounters in AGN disks can lead to asymmetry between prograde and retrograde BBH mergers. The direction of the hardening asymmetry depends on the initial binary semimajor axis. Under the assumption that the spin of the BHs becomes aligned with the angular momentum of the disk on a short timescale compared with the encounter timescale, an asymmetric distribution of mass-weighted projected spin χ eff is predicted in LIGO–Virgo detections of BBH mergers from AGN disks. In particular, this model predicts that positive χ eff BBH mergers are most likely for encounters with massive tertiaries in migration traps at radial distances ≳500–600 gravitational radii.

scholarly journals Infrared effects in the late stages of black hole evaporation

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Éanna É. Flanagan
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Center Of Mass ◽  
Planck Scale ◽  
Black Hole Mass ◽  
Order Unity ◽  
Intrinsic Angular Momentum ◽  
Hole Position ◽  
Late Stages ◽  
Shear Tensor

Abstract As a black hole evaporates, each outgoing Hawking quantum carries away some of the black holes asymptotic charges associated with the extended Bondi-Metzner-Sachs group. These include the Poincaré charges of energy, linear momentum, intrinsic angular momentum, and orbital angular momentum or center-of-mass charge, as well as extensions of these quantities associated with supertranslations and super-Lorentz transformations, namely supermomentum, superspin and super center-of-mass charges (also known as soft hair). Since each emitted quantum has fluctuations that are of order unity, fluctuations in the black hole’s charges grow over the course of the evaporation. We estimate the scale of these fluctuations using a simple model. The results are, in Planck units: (i) The black hole position has a uncertainty of $$ \sim {M}_i^2 $$ ∼ M i 2 at late times, where Mi is the initial mass (previously found by Page). (ii) The black hole mass M has an uncertainty of order the mass M itself at the epoch when M ∼ $$ {M}_i^{2/3} $$ M i 2 / 3 , well before the Planck scale is reached. Correspondingly, the time at which the evaporation ends has an uncertainty of order $$ \sim {M}_i^2 $$ ∼ M i 2 . (iii) The supermomentum and superspin charges are not independent but are determined from the Poincaré charges and the super center-of-mass charges. (iv) The supertranslation that characterizes the super center-of-mass charges has fluctuations at multipole orders l of order unity that are of order unity in Planck units. At large l, there is a power law spectrum of fluctuations that extends up to l ∼ $$ {M}_i^2/M $$ M i 2 / M , beyond which the fluctuations fall off exponentially, with corresponding total rms shear tensor fluctuations ∼ MiM−3/2.

scholarly journals Optimization of model independent gravitational wave search for binary black hole mergers using machine learning

2021 ◽  
Vol 104 (2) ◽  
Author(s):  
T. Mishra ◽  
B. O’Brien ◽  
V. Gayathri ◽  
M. Szczepańczyk ◽  
S. Bhaumik ◽  
...  
Keyword(s):  
Machine Learning ◽  
Black Hole ◽  
Gravitational Wave ◽  
Binary Black Hole ◽  
Model Independent
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