Stability and Quasi Normal Modes of Charged Born–Infeld Black Holes

Fernando, Sharmanthie; Holbrook, Chad

doi:10.1007/s10773-005-9024-9

Cited by 43 publications

(44 citation statements)

References 37 publications

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“…The properties of QNM behaviors for the second Einstein-aether black hole with c 13 are similar to the scalar and gravitational field QNMs of Einstein-Born-Infeld black holes with the Born-Infeld parameter b [32] and, the scalar, gravitational, electromagnetic and Dirac fields QNMs of noncommutative Schwarzschild black hole [38] with the spacetime noncommutative parameter ϑ. In this case, LV in gravity sector affects spacetime mass and will make quasinormal ringing of black holes damping more slowly and its period becoming longer.…”

Section: Discussionmentioning

confidence: 66%

Gravitational quasinormal modes of black holes in Einstein-aether theory

Ding

2019

Nuclear Physics B

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The local Lorentz violation (LV) in gravity sector should show itself in derivation of the characteristic quasinormal modes (QNMs) of black hole mergers from their general relativity case. In this paper, I study QNMs of the gravitational field perturbations to Einstein-aether black holes and, at first compare them to those in Schwarzschild black hole, and then some other known LV gravity theories. By comparing to Schwarzschild black hole, the first kind aether black holes have larger damping rate and the second ones have lower damping rate. And they all have smaller real oscillation frequency of QNMs. By comparing to some other LV theories, the QNMs of the first kind aether black hole are similar to that of the QED-extension limit of standard model extension, non-minimal coupling to Einstein's tensor and massive gravity theories. While as to the second kind aether black hole, they are similar to those of the noncommutative gravity theories and Einstein-Born-Infeld theories. These similarities may imply that LV in gravity sector and LV in matter sector have some intrinsic connections.

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Section: Discussionmentioning

confidence: 66%

Gravitational quasinormal modes of black holes in Einstein-aether theory

Ding

2019

Nuclear Physics B

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“…The imaginary part becomes more and more negative with the electric charge, and less and less negative with the angular momentum, like in the RN case [82]. Notice that the characteristic minimum of the imaginary part (or maximum if one plots −Im(ω) versus q) for a certain value of the electric charge close to its extremal value is observed, like in the RN case (also observed in [76] for charged BHs in the EpM theory) and contrary to Born-Infeld NLE and Gauss-Bonnet gravity, where the imaginary part is a monotonic function of the electric charge [71,72].…”

Section: Numerical Resultsmentioning

confidence: 87%

“…For previous similar works see e.g. [68][69][70][71][72][73], and for more recent works see e.g. [43,[74][75][76][77], and references therein.…”

Section: Numerical Resultsmentioning

confidence: 99%

Quasinormal modes of regular black holes with non-linear electrodynamical sources

Panotopoulos

Rincón

2019

Eur. Phys. J. Plus

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We compute the spectrum of quasinormal frequencies of regular black holes obtained in the presence of Non-Linear Electrodynamics. In particular, we perturb the black hole with a minimally coupled massive scalar field, and we study the corresponding perturbations adopting the 6th order WKB approximation. We analyze in detail the impact on the spectrum of the charge of the black hole, the quantum number of angular momentum and the overtone number. All modes are found to be stable. Finally, a comparison with other charged black holes is made, and an analytical expression for the quasinormal spectrum in the eikonal limit is provided. PACS. XX.XX.XX No PACS code given 1 IntroductionAlthough black holes (BHs) and gravitational waves (GWs) are predicted to exist within the framework of Einstein's General Relativity (GR) [1], until a few years ago there was only indirect evidence for the existence of both of them. Galactic centres are supposed to host supermassive BHs [2-4], while gravitational waves had been indirectly seen in orbital decay of binary systems due to emission of gravitational radiation [5]. The historical LIGO direct detection of GWs [6-8] has provided the strongest evidence so far that BHs do exist in Nature and that they merge, and it has opened a completely new window to the Universe. Despite the fact that BHs are the simplest objects in the Universe, characterized entirely by a handful of parameters, such as mass, spin and charges, they are fascinating objects bringing together many different areas, from gravitation to thermodynamics to quantum mechanics, and they are of paramount importance to gravitation, since they have the potential of revealing (at least) some of the hidden secrets of quantum gravity.A special attention is devoted to non-linear electrodynamics (NLE), which has a long history and it has been studied over the years in several different contexts. Maxwell's classical theory is based on a system of linear equations, but when quantum effects are taken into account, the effective equations become non-linear. The first models go back to the 30's when Euler and Heisenberg obtained QED corrections [9], while Born and Infeld obtained a finite self-energy of point-like charges [10]. Furthermore, a non-trivial extension of Maxwell's theory leads to the by now well-known Einstein-power-Maxwell (EpM) theory described by a Lagrangian density of the form L(F ) = F k , where F is the usual Maxwell invariant, to be defined below, and k is an arbitrary rational number. This class of theories maintain the nice properties of conformal invariance in any number of space time dimensionality D provided that k = D/4. Black hole solutions in (1+2)-dimensional and higher-dimensional EpM theories have been obtained in [11] and [12] respectively (see also [13,14] for scale-dependent black holes in the presence of EpM NLE). More exotic NLE models, such as logarithmic [15], rational [16], and exponential [17] among others, have been studied in connection to black hole physics.Furthermore, the well-known Reissn...

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“…For an incomplete list see e.g. [97][98][99][100][101][102], and for more recent works [103][104][105][106][107], and references therein. The QN frequencies are given by where n = 0, 1, 2... is the overtone number, ν = n + 1/2, V 0 is the maximum of the effective potential, V 0 is the second derivative of the effective potential evaluated at the maximum, while Λ(n), Ω(n) are complicated expressions of ν and higher derivatives of the potential evaluated at the maximum, and can be seen e.g.…”

Section: Numerical Resultsmentioning

confidence: 99%