QUASINORMAL MODES OF THE SCHWARZSCHILD BLACK HOLE WITH ARBITRARY SPIN FIELDS: NUMERICAL ANALYSIS

2006 ◽  
Vol 21 (35) ◽  
pp. 2671-2683 ◽  
Author(s):  
QIYUAN PAN ◽  
JILIANG JING
Keyword(s):  
Black Hole ◽  
Quantum Number ◽  
Imaginary Part ◽  
Quasinormal Modes ◽  
Arbitrary Spin ◽  
Schwarzschild Black Hole ◽  
Surprising Effect ◽  
Spin Number ◽  
Spin Fields ◽  
Angular Quantum Number

The quasinormal modes (QNMs) associated with the decay of massless arbitrary spin fields around a Schwarzschild black hole are investigated by using the continued fraction method in a united form and their universal properties are found. It is shown that these QNMs become evenly spaced for large angular quantum number l (for the boson perturbations) and j (for the fermion perturbations) and the spacing is given by [Formula: see text] which is independent of the spin number s and overtone number n, and in the complex plane they have an interesting trend which depends on n before they become the same value with the increasing l (or j). The distribution of the QNMs with arbitrary spin fields for large values l (or j) and small n can be expressed as [Formula: see text]. It is also shown that the angular quantum number has the surprising effect of increasing real part of the QNMs, but it almost does not affect the imaginary part, especially for the lowest lying mode. In addition, the spacing for imaginary part of the QNMs at high overtones is equidistant and equals to -i/4M, which is independent of l (or j) and s.

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 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.

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