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.

BLACK HOLE AREA SPECTRUM AND ENTROPY SPECTRUM VIA QUASINORMAL MODES IN A QUANTUM CORRECTED SPACETIME

2011 ◽  
Vol 26 (39) ◽  
pp. 2963-2971 ◽  
Author(s):  
CHENG-ZHOU LIU
Keyword(s):  
Black Hole ◽  
Imaginary Part ◽  
Quasinormal Modes ◽  
Area Spectrum ◽  
Entropy Spectrum ◽  
Schwarzschild Black Hole ◽  
The Real ◽  
Hole Area ◽  
Test Particles ◽  
Proper Frequency

The area spectrum and entropy spectrum of the modified Schwarzschild black hole in gravity's rainbow are investigated via the quasinormal modes of the black hole. Using the modified Hod's method and Kunstatter's method that employ the proper frequency from the imaginary part other than the real part of the quasinormal modes, the area and entropy spacing of the black hole are calculated. The results obtained from these two methods agree with each other and the equally spaced area and entropy spectrum are derived. The obtained area and entropy spectrum are independent of the energies of test particles and are the same as from the usual Schwarzschild black hole.

CAN WE DIFFERENTIATE NEUTRINOS FROM ANTI-NEUTRINOS IN EVOLUTION OF MASSLESS DIRAC FIELDS IN SCHWARZSCHILD BLACK-HOLE BACKGROUND?

2006 ◽  
Vol 21 (07) ◽  
pp. 593-601
Author(s):  
JILIANG JING
Keyword(s):  
Black Hole ◽  
Decay Rate ◽  
Power Law ◽  
Quasinormal Modes ◽  
Tail Behavior ◽  
Schwarzschild Black Hole ◽  
Dirac Fields ◽  
Black Hole Background ◽  
Opposite Chirality

We study analytically the evolution of massless Dirac fields in the background of the Schwarzschild black hole. It is shown that although the quasinormal frequencies are the same for opposite chirality with the same |k|, we can differentiate neutrinos from anti-neutrinos in evolution of the massless Dirac fields provided we know both stages for the quasinormal modes and the power-law tail behavior since the decay rate of the neutrinos is described by t-(2|k|+1) while anti-neutrinos is t-(2|k|+3).

scholarly journals Greybody factor and quasinormal modes of Regular Black Holes

2020 ◽  
Vol 80 (10) ◽  
Author(s):  
Ángel Rincón ◽  
Victor Santos
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Angular Momentum ◽  
Classical Solution ◽  
Quantum Number ◽  
Quasinormal Modes ◽  
Wkb Method ◽  
Regular Black Hole ◽  
Gravitational Perturbations ◽  
Black Hole Solutions

AbstractIn this work, we investigate the quasinormal frequencies of a class of regular black hole solutions which generalize Bardeen and Hayward spacetimes. In particular, we analyze scalar, vector and gravitational perturbations of the black hole with the semianalytic WKB method. We analyze in detail the behaviour of the spectrum depending on the parameter p/q of the black hole, the quantum number of angular momentum and the s number. In addition, we compare our results with the classical solution valid for $$p = q = 1$$ p = q = 1 .

scholarly journals QUASINORMAL MODES AND LATE-TIME TAILS OF CANONICAL ACOUSTIC BLACK HOLES

2007 ◽  
Vol 16 (07) ◽  
pp. 1211-1218 ◽  
Author(s):  
PING XI ◽  
XIN-ZHOU LI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Propagation ◽  
Angular Momentum ◽  
Numerical Method ◽  
Time Scale ◽  
Quasinormal Modes ◽  
Late Time ◽  
Classical Wave ◽  
Acoustic Black Holes

In this paper, we investigate the evolution of classical wave propagation in the canonical acoustic black hole by a numerical method and discuss the details of the tail phenomenon. The oscillating frequency and damping time scale both increase with the angular momentum l. For lower l, numerical results show the lowest WKB approximation gives the most reliable result. We also find that the time scale of the interim region from ringing to tail is not affected obviously by changing l.

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