Gravitational wave emission from a companion black hole in presence of an accretion disk around a super-massive Kerr black hole

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.

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

International Journal of Modern Physics D ◽

10.1142/s0218271814300225 ◽

2014 ◽

Vol 23 (10) ◽

pp. 1430022 ◽

Cited By ~ 50

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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Testing Gravity Theory With Extreme Mass-Ratio Inspirals: Recent Progress

Proceedings ◽

10.3390/proceedings2019017011 ◽

2019 ◽

Vol 17 (1) ◽

pp. 11

Author(s):

Shucheng Yang ◽

Shuo Xin ◽

Chen Zhang ◽

Wenbiao Han

Keyword(s):

Black Hole ◽

Gravitational Wave ◽

Recent Progress ◽

Central Body ◽

Low Frequency ◽

Kerr Black Hole ◽

Compact Object ◽

Wave Dispersion ◽

Gravity Theory ◽

Mass Ratio

A compact object captured by a supermassive black hole, named as extreme-mass-ratio inspiral (EMRI), is one of the most important gravitational wave sources for low-frequency interferometers such as LISA, Taiji, and TianQin. EMRIs can be used to accurately map the space-time of the central massive body. In the present paper, we introduce our recent progress on testing gravity theory with EMRIs. We demonstrate how to constrain gravitational wave dispersion and measure the deviation of the central body from the Kerr black hole. By using binary-EMRIs, the gravitational recoil and mass loss due to merger will be measured in a higher accuracy compared with the current LIGO observations. All these potential constrains and measurements will be useful for test of the gravity theory.

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