scholarly journals RADIATIVELY INEFFICIENT ACCRETION FLOWS INDUCED BY GRAVITATIONAL-WAVE EMISSION BEFORE MASSIVE BLACK HOLE COALESCENCE

2010 ◽  
Vol 726 (1) ◽  
pp. L14 ◽  
Author(s):  
Kimitake Hayasaki
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Massive Black Hole ◽  
Accretion Flows ◽  
Wave Emission

scholarly journals Relativistic loss cone dynamics: Infall and inspiral rates and branching ratios

2016 ◽  
Vol 12 (S324) ◽  
pp. 99-106
Author(s):  
Tal Alexander
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Stellar Dynamics ◽  
Branching Ratios ◽  
Tidal Disruption ◽  
Massive Black Hole ◽  
Loss Cone ◽  
Recent Advances ◽  
Wave Emission ◽  
Gradual Decay

AbstractI describe recent advances in the formulation and modeling of relativistic stellar dynamics around a massive black hole, and the implications for the rates of infall (e.g. tidal disruption) and inspiral (e.g. gradual decay by gravitational wave emission) processes, and their branching ratios.

scholarly journals MASSIVE BLACK HOLE BINARY SYSTEMS IN HIERARCHIAL SCENARIO OF STRUCTURE FORMATION

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1271-1274
Author(s):  
E. S. PEREIRA ◽  
O. D. MIRANDA
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Structure Formation ◽  
Binary Systems ◽  
Initial Study ◽  
Massive Black Hole ◽  
Massive Black Holes ◽  
The Press ◽  
Future Extension ◽  
Merger Rate

The hierarchical scenario of structure formation describes how objects like galaxies and galaxy clusters are formed by mergers of small objects. In this scenario, mergers of galaxies can lead to the formation of massive black hole (MBH) binary systems. On the other hand, the merger of two MBH could produce a gravitational wave signal detectable, in principle, by the Laser Interferometer Space Antenna (LISA). In the present work, we use the Press–Schechter formalism, and its extension, to describe the merger rate of haloes which contain massive black holes. Here, we do not study the gravitational wave emission of these systems. However, we present an initial study to determine the number of systems formed via mergers that could permit, in a future extension of this work, the calculation of the signature in gravitational waves of these systems.

BLACK HOLE NONEXTENSIVE ENTROPY: FORMATION PROCESSES SIGNALIZED BY GRAVITATIONAL WAVE EMISSION

2008 ◽  
Vol 17 (03n04) ◽  
pp. 541-544 ◽  
Author(s):  
H. P. DE OLIVEIRA ◽  
I. DAMIÃO SOARES
Keyword(s):  
Black Hole ◽  
Distribution Function ◽  
Gravitational Wave ◽  
Linear Approximation ◽  
Maximum Entropy Principle ◽  
Nonextensive Entropy ◽  
Entropy Principle ◽  
Wave Emission ◽  
Entropic Index ◽  
Thermodynamic Processes

We show that gravitational wave emission, both in the linear approximation and in the full nonlinear regime of general relativity, gives a hint of black hole thermodynamic processes by which a black hole evolves emitting part of its perturbation in the form of gravitational waves and absorbing the remnant, reaching a final configuration with a larger entropy. The partition of energy in this process is constrained by the maximum entropy principle, and the final entropy obtained numerically is given as a distribution function of the efficiency of the process. The distribution function is in the realm of nonextensive thermostatistics with entropic index q ≃ 1/2, a result that is validated analytically by the linear approximation.

scholarly journals The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational-wave Observatories

2021 ◽  
Vol 923 (2) ◽  
pp. 139
Author(s):  
Fupeng Zhang ◽  
Xian Chen ◽  
Lijing Shao ◽  
Kohei Inayoshi
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Signal To Noise Ratio ◽  
Galactic Nuclei ◽  
Signal To Noise ◽  
High Eccentricity ◽  
Massive Black Hole ◽  
Binary Black Holes ◽  
Binary Black Hole ◽  
Space Observatories

Abstract We study the stellar binary black holes (BBHs) inspiraling/merging in galactic nuclei based on our numerical method GNC. We find that 3%–40% of all newborn BBHs will finally merge due to various dynamical effects. In a five-year mission, up to 104, 105, and ∼100 of BBHs inspiraling/merging in galactic nuclei can be detected with signal-to-noise ration >8 in Advanced LIGO (aLIGO), Einstein/DECIGO, and TianQin/LISA/TaiJi, respectively. Roughly tens are detectable in both LISA/TaiJi/TianQin and aLIGO. These BBHs have two unique characteristics. (1) Significant eccentricities: 1%–3%, 2%–7%, or 30%–90% of them have e i > 0.1 when they enter into aLIGO, Einstein, or space observatories, respectively. Such high eccentricities provide a possible explanation for that of GW190521. Most highly eccentric BBHs are not detectable in LISA/Tianqin/TaiJi before entering into aLIGO/Einstein, as their strain becomes significant only at f GW ≳ 0.1 Hz. DECIGO becomes an ideal observatory to detect those events, as it can fully cover the rising phase. (2) Up to 2% of BBHs can inspiral/merge at distances ≲103 r SW from the massive black hole, with significant accelerations, such that the Doppler phase drift of ∼10–105 of them can be detected with signal-to-noise ratio >8 in space observatories. The energy density of the gravitational-wave backgrounds (GWBs) contributed by these BBHs deviates from the power-law slope of 2/3 at f GW ≲ 1 mHz. The high eccentricity, significant accelerations, and the different profile of the GWB of these sources make them distinguishable, and thus interesting for future gravitational-wave detections and tests of relativities.

scholarly journals The overlap of numerical relativity, perturbation theory and post-Newtonian theory in the binary black hole problem

2014 ◽  
Vol 23 (10) ◽  
pp. 1430022 ◽  
Author(s):  
Alexandre Le Tiec
Keyword(s):  
Black Hole ◽  
Perturbation Theory ◽  
Gravitational Wave ◽  
Numerical Relativity ◽  
Approximation Schemes ◽  
Newtonian Theory ◽  
Binary Black Holes ◽  
Black Hole Binaries ◽  
Physical Problems ◽  
Wave Emission

Inspiralling and coalescing binary black holes are promising sources of gravitational radiation. The orbital motion and gravitational-wave emission of such system can be modeled using a variety of approximation schemes and numerical methods in general relativity: The post-Newtonian (PN) formalism, black hole perturbation theory (BHP), numerical relativity (NR) simulations and the effective one-body (EOB) model. We review recent work at the multiple interfaces of these analytical and numerical techniques, emphasizing the use of coordinate-invariant relationships to perform meaningful comparisons. Such comparisons provide independent checks of the validity of the various calculations, they inform the development of a universal, semi-analytical model of the binary dynamics and gravitational-wave emission and they help to delineate the respective domains of validity of each approximation method. For instance, several recent comparisons suggest that perturbation theory may find applications in a broader range of physical problems than previously thought, including the radiative inspiral of intermediate mass-ratio and comparable-mass black hole binaries.

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