Gravitational wave emission from matter accretion onto a Schwarzschild black hole

2005 ◽  
Author(s):  
Alessandro Nagar
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Schwarzschild Black Hole ◽  
Wave Emission

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 Spinning test body orbiting around a Schwarzschild black hole: Circular dynamics and gravitational-wave fluxes

2016 ◽  
Vol 94 (10) ◽  
Author(s):  
Enno Harms ◽  
Georgios Lukes-Gerakopoulos ◽  
Sebastiano Bernuzzi ◽  
Alessandro Nagar
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Test Body ◽  
Schwarzschild Black Hole

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.

STABILITY OF SCHWARZSCHILD BLACK HOLE IN THE MASSIVE BRANS-DICKE THEORY

1986 ◽  
Vol 01 (03) ◽  
pp. 709-729 ◽  
Author(s):  
O.J. KWON ◽  
Y.D. KIM ◽  
Y.S. MYUNG ◽  
B.H. CHO ◽  
Y.J. PARK
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Gravitational Wave ◽  
Scalar Wave ◽  
Schwarzschild Black Hole ◽  
The Real ◽  
Gravitational Perturbations ◽  
Scalar Perturbations

For the nontachyonic mass (c<0, µ2<6), we have found that all nonstatic perturbations (odd-, even-parity and scalar perturbations) allow only the real values of frequency k. This means that the black hole in the massive Brans-Dicke theory is classically stable. However, for the tachyonic mass of scalar field (c>0, µ2>6), we find that the massive Brans-Dicke theory is classically unstable. We also emphasize that the potential forms of odd-parity perturbations is simply given by the pure-gravitational perturbations. For the even-parity case, we obtain the same potential just as Zerilli’s case by combining the even-parity gravitational wave and scalar wave. For static perturbations (k=0) and c>0, only the odd- and even-parity cases with L=0, 1 is allowed to avoid exponentially growing modes.

scholarly journals On the gamma-ray burst – gravitational wave association in GW150914

2016 ◽  
Vol 12 (S324) ◽  
pp. 291-294
Author(s):  
Agnieszka Janiuk ◽  
Szymon Charzynski ◽  
Michal Bejger
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Gamma Ray ◽  
Photon Emission ◽  
Close Binary ◽  
Wave Source ◽  
Compact Binary ◽  
Electron Positron ◽  
Wave Emission ◽  
Prompt Emission

AbstractHyperaccreting disks around black holes are the engines that drive outflows and jets in gamma ray bursts (GRBs). The torus formed after the core collapse or a compact binary merger is composed of free nucleons, Helium, electron-positron pairs, and is cooled by neutrinos rather than photon emission. Hyperaccretion powers the ultra-relativistic jets, where the GRB prompt emission originates. The neutrons produced in the disk and also in the outflowing material are necessary for the production of heavier nuclei. We discuss here the observable consequences of nucleosynthesis and we also apply the scenario of hyperaccretion to the gravitational wave source, GW150914. Temporal coincidence reported by the Fermi satellite suggested that the black hole merger might be accompanied with a GRB. We propose that a collapsing massive star and a black hole in a close binary could lead to such event. Gravitational wave emission due to the merger of collapsed core and the companion black hole might then coincide with a weak GRB.

scholarly journals Post-merger Jets from Supermassive Black Hole Coalescences as Electromagnetic Counterparts of Gravitational Wave Emission

2021 ◽  
Vol 911 (1) ◽  
pp. L15
Author(s):  
Chengchao Yuan ◽  
Kohta Murase ◽  
B. Theodore Zhang ◽  
Shigeo S. Kimura ◽  
Péter Mészáros
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Supermassive Black Hole ◽  
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.

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