scholarly journals General theories of linear gravitational perturbations to a Schwarzschild black hole

2018 ◽  
Vol 97 (4) ◽  
Author(s):  
Oliver J. Tattersall ◽  
Pedro G. Ferreira ◽  
Macarena Lagos
Keyword(s):  
Black Hole ◽  
Schwarzschild Black Hole ◽  
Gravitational Perturbations

scholarly journals QUASI-NORMAL MODES OF SCHWARZSCHILD–ANTI-DE SITTER BLACK HOLES: ELECTROMAGNETIC AND GRAVITATIONAL PERTURBATIONS

2002 ◽  
Vol 17 (20) ◽  
pp. 2752-2752
Author(s):  
VITOR CARDOSO ◽  
JOSÉ P. S. LEMOS
Keyword(s):  
Black Hole ◽  
Imaginary Part ◽  
Normal Modes ◽  
De Sitter ◽  
Schwarzschild Black Hole ◽  
Small Black Hole ◽  
Conformal Field ◽  
Gravitational Perturbations ◽  
Ads Spacetime ◽  
Electromagnetic Perturbation

We studied the quasi-normal modes (QNM) of electromagnetic and gravitational perturbations of a Schwarzschild black hole in an asymptotically anti-de Sitter (AdS) spacetime, extending previous works1,2 on the subject. Some of the electromagnetic modes do not oscillate, they only decay, since they have pure imaginary frequencies. The gravitational modes show peculiar features: the odd and even gravitational perturbations no longer have the same characteristic quasinormal frequencies. There is a special mode for odd perturbations whose behavior differs completely from the usual one in scalar1 and electromagnetic perturbation in an AdS spacetime, but has a similar behavior to the Schwarzschild black hole3 in an asymptotically flat spacetime: the imaginary part of the frequency goes as [Formula: see text], where r+ is the horizon radius. We also investigated the small black hole limit showing that the imaginary part of the frequency goes as [Formula: see text]. These results are important to the AdS/CFT4 conjecture since according to it the QNMs describe the approach to equilibrium in the conformal field theory. For other geometries see5,6.

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 Probing the parameters of a Schwarzschild black hole surrounded by quintessence and cloud of strings through four standard astrophysical tests

2021 ◽  
Vol 81 (10) ◽  
Author(s):  
Víctor H. Cárdenas ◽  
Mohsen Fathi ◽  
Marco Olivares ◽  
J. R. Villanueva
Keyword(s):  
Black Hole ◽  
Time Delay ◽  
Observational Data ◽  
Gravitational Redshift ◽  
Schwarzschild Black Hole ◽  
Gravitational Perturbations ◽  
Deflection Of Light ◽  
Static Black Hole ◽  
Planetary Orbits ◽  
General Relativistic

AbstractIn this paper, we concern about applying general relativistic tests on the spacetime produced by a static black hole associated with cloud of strings, in a universe filled with quintessence. The four tests we apply are precession of the perihelion in the planetary orbits, gravitational redshift, deflection of light, and the Shapiro time delay. Through this process, we constrain the spacetime’s parameters in the context of the observational data, which results in about $$\sim 10^{-9}$$ ∼ 10 - 9 for the cloud of strings parameter, and $$\sim 10^{-20}$$ ∼ 10 - 20  m$$^{-1}$$ - 1 for that of quintessence. The response of the black hole to the gravitational perturbations is also discussed.

scholarly journals QUASINORMAL MODES AND LATE-TIME TAILS IN THE BACKGROUND OF SCHWARZSCHILD BLACK HOLE PIERCED BY A COSMIC STRING: SCALAR, ELECTROMAGNETIC AND GRAVITATIONAL PERTURBATIONS

2008 ◽  
Vol 23 (16n17) ◽  
pp. 2505-2524 ◽  
Author(s):  
SONGBAI CHEN ◽  
BIN WANG ◽  
RUKENG SU
Keyword(s):  
Black Hole ◽  
Electromagnetic Fields ◽  
Cosmic String ◽  
Quasinormal Modes ◽  
Late Time ◽  
Gravitational Perturbation ◽  
Schwarzschild Black Hole ◽  
Gravitational Perturbations ◽  
Test Particles

We have studied the quasinormal modes and the late-time tail behaviors of scalar, electromagnetic and gravitational perturbations in the Schwarzschild black hole pierced by a cosmic string. Although the metric is locally identical to that of the Schwarzschild black hole so that the presence of the string will not imprint in the motion of test particles, we found that quasinormal modes and the late-time tails can reflect physical signatures of the cosmic string. Compared with the scalar and electromagnetic fields, the gravitational perturbation decays slower, which would be more interesting to disclose the string effect in this background.

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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