scholarly journals Detecting gravitational waves from test-mass bodies orbiting a Kerr black hole with P-approximant templates

2005 ◽  
Vol 22 (18) ◽  
pp. S1211-S1221
Author(s):  
Edward K Porter
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
Test Mass

scholarly journals ON BLACK HOLE CREATION IN PLANCKIAN ENERGY SCATTERING

1996 ◽  
Vol 05 (06) ◽  
pp. 707-721 ◽  
Author(s):  
I. YA. AREF’EVA ◽  
I.V. VOLOVICH ◽  
K.S. VISWANATHAN
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Black Hole Solution ◽  
Kerr Black Hole ◽  
Energy Scattering ◽  
Light Particles ◽  
Black Hole Creation ◽  
Plane Gravitational Waves

In a series of papers Amati, Ciafaloni and Veneziano and ’t Hooft conjectured that black holes occur in the collision of two light particles at planckian energies. In this talk based on [10] we discuss a possible scenario for such a process by using the Chandrasekhar-Ferrari-Xanthopoulos duality between the Kerr black hole solution and colliding plane gravitational waves.

scholarly journals Gravitational waves in Brans-Dicke theory: Analysis by test particles around a Kerr black hole

1997 ◽  
Vol 56 (2) ◽  
pp. 785-797 ◽  
Author(s):  
Motoyuki Saijo ◽  
Hisa-aki Shinkai ◽  
Kei-ichi Maeda
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
Theory Analysis ◽  
Test Particles

scholarly journals Post-Newtonian Expansion of Gravitational Waves from a Particle in Circular Orbits around a Rotating Black Hole: Effects of Black Hole Absorption

1999 ◽  
Vol 183 ◽  
pp. 163-163
Author(s):  
Hideyuki Tagoshi ◽  
Shuhei Mano ◽  
Eiichi Takasugi
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Energy Absorption ◽  
Absorption Rate ◽  
Kerr Black Hole ◽  
Compact Binaries ◽  
Wave Forms ◽  
Teukolsky Equation ◽  
Interferometric Detectors ◽  
Near Future

Coalescing compact binaries are the most promising candidates for detection by near-future, ground based laser interferometric detectors. It is very important to investigate detailed wave forms from coalescing compact binaries. When one (or two) of the stars is a black hole, some of those waves are absorbed by the black hole. Here, we consider a case when a test particle moves circular orbit on the equatorial plane around a Kerr black hole, and calculate the the energy absorption rate by the black hole. We adopt an analytic techniques for the Teukolsky equation which was found by Mano, Suzuki, and Takasugi (1996). We calculated the energy absorption rate to O((v/c)13) beyond the Newtonian-quadrupole formula of gravitational waves radiated to infinity, assuming v/c ≪ 1. Here v is the velocity of the particle. We find that, when a black hole is rotating, the black hole absorption appear at O((v/c)5) beyond the Newtonian-quadrapole formula. These effects become more important as the mass of the black hole becomes larger. We also found that the black hole absorption is more important when a particle moves to the same direction of the black hole rotation. All the details of this paper is presented in Tagoshi et al. (1997).

Gravitational waves from a spinning particle plunging into a Kerr black hole

1998 ◽  
Vol 58 (6) ◽  
Author(s):  
Motoyuki Saijo ◽  
Kei-ichi Maeda ◽  
Masaru Shibata ◽  
Yasushi Mino
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
Spinning Particle

scholarly journals Amplification of Waves Reflected from Kerr Black Holes

1974 ◽  
Vol 64 ◽  
pp. 94-94 ◽  
Author(s):  
A. A. Starobinsky
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Quantum Effect ◽  
Kerr Black Hole ◽  
Kerr Metric ◽  
Black Hole Mass ◽  
Quantum Version ◽  
Penrose Process ◽  
The One ◽  
Energy And Momentum

The effect of amplification of electromagnetic and gravitational waves reflected from a rotating black hole (‘superradiance scattering’) is investigated. This effect was proposed by Zel'dovich (1971). It leads, as well as the Penrose process, to the energy extraction from a Kerr black hole at the expense of its rotational energy and momentum decrease. The coefficient of wave reflection R>1 if ω<nω, where ω is the wave frequency, n - its angular momentum and ω is the black hole angular velocity. The value of this effect is not small in the case of gravitational waves, for example, if l=n = 2, ω →nω and a = M, then R≈2.38.There also exists a quantum version of the effect, namely, the one of spontaneous pair creation in the Kerr metric, but this quantum effect is exceedingly small in real astrophysical conditions, because its characteristic time is of the order G2M3/hc4, where M is the black hole mass.

On algebraically special perturbations of black holes

1984 ◽  
Vol 392 (1802) ◽  
pp. 1-13 ◽  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Special Class ◽  
Mathematical Theory ◽  
Kerr Black Hole ◽  
Potential Barriers

Algebraically special perturbations of black holes excite gravitational waves that are either purely ingoing or purely outgoing. Solutions, appropriate to such perturbations of the Kerr, the Schwarzschild, and the Reissner-Nordström black-holes, are obtained in explicit forms by different methods. The different methods illustrate the remarkable inner relations among different facets of the mathematical theory. In the context of the Kerr black-hole they derive from the different ways in which the explicit value of the Starobinsky constant emerges, and in the context of the Schwarzschild and the Reissner-Nordström black-holes they derive from the potential barriers surrounding them belonging to a special class.

On the equations governing the axisymmetric perturbations of the Kerr black hole

1975 ◽  
Vol 345 (1641) ◽  
pp. 145-167 ◽  
Keyword(s):  
Black Hole ◽  
Wave Equation ◽  
Conservation Laws ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
One Dimensional ◽  
Potential Barriers ◽  
Transmission Coefficients ◽  
Dimensional Wave ◽  
Axisymmetric Perturbations

It is shown how Teukolsky’s equation, governing the perturbations of the Kerr black hole, can be reduced, in the axisymmetric case, to a one-dimensional wave equation with four possible potentials. The potentials are implicitly, dependent on the frequency; and besides, depending on circumstances, they can be complex. In all cases (i.e. whether or not the potentials are real or complex), the problem of the reflexion and the transmission of gravitational waves by the potential barriers can be formulated, consistently, with the known conservation laws. It is, further, shown that all four potentials lead to the same reflexion and transmission coefficients.

scholarly journals Weighing the black hole via quasi-local energy

2017 ◽  
Vol 32 (24) ◽  
pp. 1730021 ◽  
Author(s):  
Yuan K. Ha
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
Rotational Energy ◽  
Local Energy ◽  
External Energy ◽  
Event Horizons ◽  
Binary Black Hole ◽  
Asymptotic Values

We set to weigh the black holes at their event horizons in various spacetimes and obtain masses which are substantially higher than their asymptotic values. In each case, the horizon mass of a Schwarzschild, Reissner–Nordström, or Kerr black hole is found to be twice the irreducible mass observed at infinity. The irreducible mass does not contain electrostatic or rotational energy, leading to the inescapable conclusion that particles with electric charges and spins cannot exist inside a black hole. This is proposed as the External Energy Paradigm. A higher mass at the event horizon and its neighborhood is obligatory for the release of gravitational waves in binary black hole merging. We describe how these horizon mass values are obtained in the quasi-local energy approach and applied to the black holes of the first gravitational waves GW150914.

On the reflexion and transmission of neutrino waves by a Kerr black hole

1977 ◽  
Vol 352 (1670) ◽  
pp. 325-338 ◽  
Keyword(s):  
Black Hole ◽  
Wave Equation ◽  
Gravitational Waves ◽  
Kerr Black Hole ◽  
One Dimensional ◽  
Potential Barriers ◽  
Two Component ◽  
Reflexion Coefficient ◽  
Dimensional Wave

The equations governing the two-component neutrino are reduced to the form of a one-dimensional wave equation. And it is shown how the absence of super-radiance (i. e. a reflexion coefficient in excess of one) for incident neutrino waves and its manifestation for incident electromagnetic and gravitational waves (of suitable frequencies) emerge very naturally from the character of the respective potential barriers that surround the Kerr black hole.

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