Black holes in nonlinear electrodynamics: Quasinormal spectra and parity splitting

Chaverra, Eliana; Degollado, Juan Carlos; Moreno, Claudia; Sarbach, Olivier

doi:10.1103/physrevd.93.123013

Cited by 28 publications

(32 citation statements)

References 56 publications

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“…One can see from (42) that the existence of the Schwarzschild mass does not effect the energy conditions of these black holes, since only derivatives of the ρ 2 with respect to radial coordinate appear in energy-momentum tensor. According to the WEC, T µν u µ u ν ≥ 0 where u µ is the generic timelike vector, or T (0)(0) ≥ 0 and It is well known that in general relativity (GR) there are two types of singularities which are the points where the spacetime metric coefficients tend to infinity: curva-ture singularity which is often called a physical singularity by the reason of that it cannot be removed by coordinate transformations, while the second one is the coordinate singularity (event horizon) which can be considered as a mathematical singularity due to the possibility of elimination of it by introducing appropriate coordinate system.…”

Section: Energy Conditionsmentioning

confidence: 97%

“…A detailed discussion of the circular geodesics of the regular Bardeen and Ayon-Beato-Garcia (ABG) black hole and no-horizon spacetimes and its implication to simple optical phenomena can be found in [31]. Moreover, scalar, electromagnetic and gravitational perturbations of the regular black holes in nonlinear electrodynamics, their quasinormal modes and stabilities have been discussed in several works, see for instance [37][38][39][40][41][42]. Note that the geodesic structure of the regular black holes outside the horizon is similar to those of the Schwarzschild or Reissner-Nordström (RN) black hole spacetimes, but under the inner horizon, no circular geodesics can exist.…”

Section: Introductionmentioning

confidence: 99%

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Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

2017

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We construct regular rotating black hole and no-horizon spacetimes based on the recently introduced spherically symmetric generic regular black hole spacetimes related to electric or magnetic charge under nonlinear electrodynamics coupled to general relativity that for special values of the spacetime parameters reduce to the Bardeen and Hayward spacetimes. We show that the weak and strong energy conditions are violated inside the Cauchy horizons of these generic rotating black holes. We give the boundary between the rotating black hole and no-horizon spacetimes and determine the black hole horizons and the boundary of the ergosphere. We introduce the separated Carter equations for the geodesic motion in these rotating spacetimes. For the most interesting new class of the regular spacetimes, corresponding for magnetic charges to the Maxwell field in the weak field limit of the nonlinear electrodynamics, we determine the structure of the circular geodesics and discuss their properties. We study the epicyclic motion of a neutral particle moving along the stable circular orbits around the "Maxwellian" rotating regular black holes. We show that epicyclic frequencies measured by the distant observers and related to the oscillatory motion of the neutral test particle along the stable circular orbits around the rotating singular and regular Maxwellian black holes are always smaller than ones in the Kerr spacetime.

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Section: Energy Conditionsmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

2017

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“…in [84]. Therefore, although in the presence of non-linear electromagnetic sources photons follow the null trajectories of an effective geometry rather than the null geodesics of the true geometry [85][86][87], the previous expressions for Ω c and for λ L remain the same. We see that the angular velocity determines the real part of the modes, where only the degree of angular momentum l enters, while the Lyapunov exponent determines the imaginary part of the modes, where only the overtone number n enters.…”

Section: Qnms In the Eikonal Limitmentioning

confidence: 93%

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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“…However, for scalar and EM perturbations, also through the typical standard analysis, similar wave equations can be obtained despite the different underlying physics. The scalar [12][13][14][15], gravitational [16,17] and EM [18,19] perturbations of regular BHs have been studied. One of the important properties of the perturbations is the relaxation time which is defined by the inverse of imaginary part of the QNMs, τ = 1/ω i .…”

Section: Introductionmentioning

confidence: 99%

“…Despite, Eqs. (15), (16), (17) are analytically not solvable, it is not difficult to check that for all values of q they always have at least one real zero (see the right panel of Fig. 2).…”

Section: Introductionmentioning

confidence: 99%

Relaxations of perturbations of spacetimes in general relativity coupled to nonlinear electrodynamics

et al. 2019

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Three well known exact regular solutions of general relativity (GR) coupled to nonlinear electrodynamics (NED), namely the Maxwellian, Bardeen and Hayward regular spacetimes, which can describe either a regular black hole or a geometry without horizons, have been considered. Relaxation times for the scalar, electromagnetic (EM) and gravitational perturbations of black holes (BHs) and no-horizon spacetimes have been estimated in comparison with the ones of the Schwarzschild and Reissner-Nordström (RN) spacetimes. It has been shown that the considered geometries in GR coupled to the NED have never vanishing circular photon orbits and on account of this fact these spacetimes always oscillate the EM perturbations with quasinormal frequencies (QNFs). Moreover we have shown that the EM perturbations in the eikonal regime can be a powerful tool to confirm that (i) the light rays do not follow null geodesics in the NED by the relaxation rates; (ii) if the underlying solution has a correct weak field limit to the Maxwell electrodynamics (LED) by the angular velocity of the circular photon orbit.

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Black holes in nonlinear electrodynamics: Quasinormal spectra and parity splitting

Cited by 28 publications

References 56 publications

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

Generic rotating regular black holes in general relativity coupled to nonlinear electrodynamics

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

Relaxations of perturbations of spacetimes in general relativity coupled to nonlinear electrodynamics

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