The gravitational perturbations of the Kerr black hole IV. The completion of the solutiont

1980 ◽  
Vol 372 (1751) ◽  
pp. 475-484 ◽  
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Space Time ◽  
Gravitational Perturbations ◽  
Kerr Space ◽  
The One

This paper eliminates the last remaining lacuna in the information that was needed to make the solution for the perturbations in the metric coefficients of the Kerr space-time fully explicit. The requisite information is obtained from a pair of equations which is complementary to the one considered in paper III; and the solution of the Newman-Penrose equations governing the perturbations is, thus, completed.

scholarly journals Shadow of a Kerr-like black hole

2014 ◽  
Vol 10 (S312) ◽  
pp. 135-136
Author(s):  
Farruh Atamurotov
Keyword(s):  
Black Hole ◽  
Angular Momentum ◽  
Deformation Parameter ◽  
Space Time ◽  
Black Hole Spin ◽  
Spin Parameter ◽  
Kerr Space ◽  
The One

AbstractThe shadow of a Kerr-like black hole has been considered and it was shown that in addition to the specific angular momentum a, deformation parameter of Kerr-like space-time essentially deforms the shape of the black hole shadow. For a given value of the black hole spin parameter a, the presence of a deformation parameter ε reduces the shadow and enlarges its deformation with respect to the one in the Kerr space-time.

The gravitational perturbations of the Kerr black hole I. The perturbations in the quantities which vanish in the stationary state

1978 ◽  
Vol 358 (1695) ◽  
pp. 421-439 ◽  
Keyword(s):  
Black Hole ◽  
Stationary State ◽  
Weyl Tensor ◽  
Kerr Black Hole ◽  
Maxwell Field ◽  
Subsequent Work ◽  
Kerr Geometry ◽  
Gravitational Perturbations ◽  
Newman Black Hole ◽  
Basic Equations

As a preliminary towards a complete integration of the Newman-Penrose equations governing the gravitational perturbations of the Kerr black hole, the perturbations in the spin coefficients and in the components of the Weyl tensor, which vanish in the stationary state, are considered. The manner of treatment of the basic equations yields Teukolsky’s equations expressed directly in terms of the basic derivative operators of the theory and, further, suggests a preferred gauge in which two of the components of the Weyl tensor are governed by the same equations as a Maxwell field. Various identities and relations that are needed in subsequent work are assembled. In two appendixes, the solution of Maxwell’s equations in Kerr geometry and the perturbations of the charged Kerr-Newman black hole are considered.

scholarly journals Kerr black hole in canonically deformed space-time

2014 ◽  
Vol 8 ◽  
pp. 1113-1123
Author(s):  
Marcin Daszkiewicz ◽  
Cezary J. Walczyk
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Space Time

scholarly journals SUPERMASSIVE BLACK HOLES OR BOSON STARS? HAIR COUNTING WITH GRAVITATIONAL WAVE DETECTORS

2006 ◽  
Vol 15 (12) ◽  
pp. 2209-2216 ◽  
Author(s):  
EMANUELE BERTI ◽  
VITOR CARDOSO
Keyword(s):  
Black Holes ◽  
Laser Interferometer ◽  
Kerr Black Hole ◽  
Space Time ◽  
Multipole Moments ◽  
Boson Stars ◽  
Laser Interferometer Space Antenna ◽  
Kerr Space ◽  
Oscillation Frequencies ◽  
Rule Out

The evidence for supermassive Kerr black holes in galactic centers is strong and growing, but only the detection of gravitational waves will convincingly rule out other possibilities to explain the observations. The Kerr space–time is completely specified by the first two multipole moments: mass and angular momentum. This is usually referred to as the "no-hair theorem," but it is really a "two-hair" theorem. If general relativity is the correct theory of gravity, the most plausible alternative to a supermassive Kerr black hole is a rotating boson star. Numerical calculations indicate that the space–time of rotating boson stars is determined by the first three multipole moments ("three-hair theorem"). The Laser Interferometer Space Antenna (LISA) could accurately measure the oscillation frequencies of these supermassive objects. We propose to use these measurements to "count their hair," unambiguously determining their nature and properties.

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.

scholarly journals GRAVITATIONAL PERTURBATIONS OF THE KERR BLACK HOLE DUE TO ARBITRARY SOURCES

2002 ◽  
Vol 11 (08) ◽  
pp. 1331-1346 ◽  
Author(s):  
CLAUDIA MORENO ◽  
DARÍO NÚÑEZ
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Weyl Tensor ◽  
Kerr Black Hole ◽  
Null Vector ◽  
Source Terms ◽  
Field Equations ◽  
Null Tetrad ◽  
Gravitational Perturbations

We describe the Kerr black hole in the ingoing and outgoing Kerr–Schild horizon penetrating coordinates. Starting from the null vector naturally defined in these coordinates, we construct the null tetrad for each case, as well as the corresponding geometrical quantities allowing us to explicitly derive the field equations for the perturbed scalar projections Ψ0(1) and Ψ4(1) of the Weyl tensor, including arbitrary source terms. This perturbative description, including arbitrary sources, described in horizon penetrating coordinates is desirable in several lines of research on black holes, and contributes to the implementation of a formalism aimed to study the evolution of the spacetime in the region where two black holes are close together.

Quantization of electromagnetic and gravitational perturbations of a Kerr black hole

1981 ◽  
Vol 24 (2) ◽  
pp. 297-304 ◽  
Author(s):  
P. Candelas ◽  
P. Chrzanowski ◽  
K. W. Howard
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Gravitational Perturbations

scholarly journals Gravitational perturbations from NHEK to Kerr

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Alejandra Castro ◽  
Victor Godet ◽  
Joan Simón ◽  
Wei Song ◽  
Boyang Yu
Keyword(s):  
Black Hole ◽  
Line Element ◽  
Kerr Black Hole ◽  
Kerr Solution ◽  
Regularity Conditions ◽  
New Developments ◽  
Gravitational Perturbations ◽  
Dynamical Properties ◽  
Complete Characterisation

Abstract We revisit the spectrum of linear axisymmetric gravitational perturbations of the (near-)extreme Kerr black hole. Our aim is to characterise those perturbations that are responsible for the deviations away from extremality, and to contrast them with the linearized perturbations treated in the Newman-Penrose formalism. For the near horizon region of the (near-)extreme Kerr solution, i.e. the (near-)NHEK background, we provide a complete characterisation of axisymmetric modes. This involves an infinite tower of propagating modes together with the much subtler low-lying mode sectors that contain the deformations driving the black hole away from extremality. Our analysis includes their effects on the line element, their contributions to Iyer-Wald charges around the NHEK geometry, and how to reconstitute them as gravitational perturbations on Kerr. We present in detail how regularity conditions along the angular variables modify the dynamical properties of the low-lying sector, and in particular their role in the new developments of nearly-AdS2 holography.

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