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1.
Quasinormal modes(QNMs) for Dirac perturbations of f(R) black holes(BHs) are described in this paper,involving two types of f(R) solution: f(R)(Schwarzschild) BHs and f(R)(Maxwell) BHs. With the finite difference method, the stability of the f(R) black holes(BHs) is analysed and the threshold range of f(R)(Schwarzschild) BHs and f(R)(Maxwell) BHs is defined respectively. The results show that due to the presence of the correction factor R0, the damping rate of Dirac field decreases. Meanwhile, the influence of angular quantum number values |k| on the f(R) BHs is investigated. The results indicate that the QNMs oscillation becomes tenser and damping speed slowly decreases with|k| increasing. Furthermore, under the Dirac perturbation, the stability of f(R) solutions can be reflected in the manner of Dirac QNMs. The relationships between the QNMs and the parameters(|k|, charge Q and mass m) are discussed in massless, and massive cases, by contrast to the classical BHs. 相似文献
2.
We provide a comprehensive survey of possible applications of the matrix method for black hole quasinormal modes. The proposed algorithm can generally be applied to various background metrics, and in particular, it accommodates both analytic and numerical forms of the tortoise coordinates, as well as black hole spacetimes. We give a detailed account of different types of black hole metrics, master equations, and the corresponding boundary conditions. Besides, we argue that the method can readily be applied to cases where the master equation is a system of coupled equations. By adjusting the number of interpolation points, the present method provides a desirable degree of precision, in reasonable balance with its efficiency. The method is flexible and can easily be adopted to various distinct physical scenarios. 相似文献
3.
Singularities of regular black holes and the monodromy method for asymptotic quasinormal modes 下载免费PDF全文
We use the monodromy method to investigate the asymptotic quasinormal modes of regular black holes based on the explicit Stokes portraits. We find that, for regular black holes with spherical symmetry and a single shape function, the analytical forms of the asymptotic frequency spectrum are not universal and do not depend on the multipole number but on the presence of complex singularities and the trajectory of asymptotic solutions along the Stokes lines. 相似文献
4.
Tong-Zheng Wang Wei-Liang Qian Juan Fernando Zapata Zapata Kai Lin 《中国物理C(英文版)》2022,46(4):045101-045101-8
This study explores the scalar and Dirac quasinormal modes pertaining to a class of black hole solutions in the scalar-tensor-Gauss-Bonnet theory. The black hole metrics in question are novel analytic solutions recently derived in the extended version of the theory, which effectively follows at the level of the action of string theory. Owing to the existence of a nonlinear electromagnetic field, the black hole solution possesses a nonvanishing magnetic charge. In particular, the metric is capable of describing black holes with distinct characteristics by assuming different values of the ADM mass and the magnetic charge. This study investigates the scalar and Dirac perturbations in these black hole spacetimes; in particular, we focus on two different types of solutions, based on distinct horizon structures. The properties of the complex frequencies of the obtained dissipative oscillations are investigated, and the stability of the metric is subsequently addressed. We also elaborate on the possible implications of this study. 相似文献
5.
A. López-Ortega 《General Relativity and Gravitation》2005,37(1):167-190
Some properties of the Hawking radiation emitted by the family of black holes of the Einstein–Maxwell–Dilaton with cosmologicalconstant theory in three dimensions found by Chan and Mann are studiedusing the complex paths method and the Damour–Ruffini method. Theexact values of the quasinormal frequencies of the massless Diracfield propagating on a particular black hole of this family arecalculated. Taking as a basis the results obtained for the values ofthe quasinormal frequencies the instability of some modes isdiscussed. The extension of these results to the black holes of theEinstein–Maxwell–Dilaton theory in four dimensions is studied in theappendix. 相似文献
6.
The prospect of using gravitational wave detections via the quasinormal modes (QNMs) to test modified gravity theories is exciting area of current research. Gravitational waves (GWs) emitted by a perturbed black hole (BH) will decay as a superposition of their QNMs of oscillations at the ringdown phase. In this work, we investigate the QNMs of the Einstein-Euler-Heisenberg (EEH) BH for both axial and polar gravitational perturbations. We obtain master equations with the tetrad formalism, and the quasinormal frequencies of the EEH BH are calculated in the 6th order Wentzel-Kramers-Brill?uin approximation. It is interesting to note that the QNMs of the EEH BH would differ from those of the Reissner-Nordstr?m BH under the EH parameter, which indicates the EH parameter would affect the gravitational perturbations for the EEH BH. 相似文献
7.
We present the quasinormal frequencies of the massive scalar field in the background of a Schwarzchild black hole surrounded
by quintessence with the third-order WKB method. The mass of the scalar field u plays an important role in studying the quasinormal frequencies, the real part of the frequencies increases linearly as mass
of the field u increases, while the imaginary part in absolute value decreases linearly which leads to damping more slowly than the massless
scalar field. The frequencies have a limited value, so it is easier to detect the quasinormal modes. Moreover, owing to the
presence of the quintessence, the massive scalar field damps more slowly.
相似文献
8.
The massless scalar quasinormal modes (QNMs) of a stationary axisymmetric
Einstein--Maxwell dilaton--axion (EMDA) black hole are calculated
numerically using the continued fraction method first proposed by
Leaver. The fundamental quasinormal frequencies
(slowly damped QNMs) are obtained and the peculiar
behaviours of them are studied. It is shown that these frequencies depend on
the dilaton parameter $D$, the rotational parameter $a$,
the multiple moment $l$ and the azimuthal number $m$,
and have the same values
with other authors at the Schwarzschild and Kerr limit. 相似文献
9.
In this paper, using the third-order WKB approximation, we
investigate the quasinormal frequencies of the scalar field in the
background of a five-dimensional Lovelock black hole. We find that the
ultraviolet correction to Einstein theory in the Lovelock theory
makes the scalar field decay more slowly and
oscillate more quickly, and the cosmological constant makes the
scalar field decay more slowly and oscillate
more slowly in the Lovelock black hole background. 相似文献
10.
Numerical studies of the coupled Einstein‐Klein‐Gordon system have recently revealed that confined scalar fields generically collapse to form caged black holes. In the light of this finding, we analytically study the characteristic resonance spectra of the confined scalar fields in rotating linear dilaton black hole geometry. Confining mirrors (cage) are assumed to be placed in the near‐horizon region of a caged rotating linear dilaton black hole ( is the radius of the cage and r2 represents the event horizon). The radial part of the Klein‐Gordon equation is written as a Schrödinger‐like wave equation, which reduces to a Bessel differential equation around the event horizon. Using analytical tools and proper boundary conditions, we obtain the boxed‐quasinormal mode frequencies of the caged rotating linear dilaton black hole. Finally, we employ Maggiore's method, which evaluates the transition frequency in the adiabatic invariant quantity from the highly damped quasinormal modes, in order to investigate the entropy/area spectra of the rotating linear dilaton black hole. 相似文献
11.
We study quasinormal modes(QNMs)of charged black holes in the Einstein-Maxwell-Weyl(EMW)gravity by adopting the test scalar field perturbation.We find that the imaginary part of QNM frequencies is consistently negative for different angular parameters l,indicating that these modes always decay and are therefore stable.We do not observe a linear relationship between the QNM frequencyωand parameter p for these black holes,as their charge Q causes a nonlinear effect.We evaluate the massive scalar field perturbation in charged black holes and find that random long lived modes(i.e.,quasiresonances)could exist in this spectrum. 相似文献
12.
A. López-Ortega 《General Relativity and Gravitation》2008,40(7):1379-1401
By using the sixth order WKB approximation we calculate for an electromagnetic field propagating in D-dimensional Schwarzschild and Schwarzschild de Sitter (SdS) black holes its quasinormal (QN) frequencies for the fundamental
mode and first overtones. We study the dependence of these QN frequencies on the value of the cosmological constant and the
spacetime dimension. We also compare with the results for the gravitational perturbations propagating in the same background.
Moreover we compute exactly the QN frequencies of the electromagnetic field propagating in D-dimensional massless topological black hole and for the charged D-dimensional Nariai spacetime we calculate exactly the QN frequencies of the coupled electromagnetic and gravitational perturbations. 相似文献
13.
14.
15.
In the framework of the gravity's rainbow, the asymptotic
quasinormal modes of the modified Schwarzschild black holes
undergoing a scalar perturbation are investigated. By using the
monodromy method, we analytically calculated the asymptotic
quasinormal frequencies, which depend on not only the mass parameter
of the black hole, but also the particle's energy of the
perturbation field. Meanwhile, the real parts of the asymptotic
quasinormal modes can be expressed as TH\ln 3, which is
consistent with Hod's conjecture. In addition, for the quantum
corrected black hole, the area spacing is independent of the
particle's energy, even though the area itself depends on the
particle's energy. And that, by relating the area spectrum to loop
quantum gravity, the Barbero-Immirzi parameter is given and it
remains the same as from the usual black hole. 相似文献
16.
Takashi Nakamura 《Proceedings of the Japan Academy. Series B, Physical and biological sciences》2006,82(9):311-327
Numerical simulations were performed for the formation process of rotating black holes. It is suggested that Kerr black holes are formed for wide ranges of initial parameters. The nature of gravitational waves from a test particle falling into a Kerr black hole as well as the development of 3D numerical relativity for the coalescing binary neutron stars are discussed. 相似文献
17.
A. López-Ortega 《General Relativity and Gravitation》2007,39(7):1011-1029
We find exact solutions to the Dirac equation in D-dimensional de Sitter spacetime. Using these solutions we analytically calculate the de Sitter quasinormal (QN) frequencies
of the Dirac field. For the massive Dirac field this computation is similar to that previously published for massive fields
of half-integer spin moving in four dimensions. However to calculate the QN frequencies of the massless Dirac field we must
use distinct methods in odd and even dimensions, therefore the computation is different from that already known for other
massless fields of integer spin. 相似文献
18.
In this Letter, we construct the quasi-normal modes of three-dimensional extremal black holes in an algebraic way. We show that the infinite towers of the quasi-normal modes of scalar, vector and tensor could be constructed as the descendents of the highest weight modes. Our investigation shows that the hidden conformal symmetry suggested in Chen et al. (2010) [5] is an intrinsic property of the extremal black hole. Moreover, we notice that we need to fix the freedom in defining the local vector fields and find the right hidden conformal symmetry to obtain the physical quasi-normal modes. 相似文献
19.
A. López-Ortega 《General Relativity and Gravitation》2006,38(12):1747-1770
Using the monodromy method we calculate the asymptotic quasinormal frequencies of an electromagnetic field moving in D-dimensional Schwarzschild and Schwarzschild de Sitter black holes (D ≥ 4). For the D-dimensional Schwarzschild anti-de Sitter black hole we also compute these frequencies with a similar method. Moreover, we calculate the electromagnetic normal modes of the D-dimensional anti-de Sitter spacetime. 相似文献
20.
Bécar Ramón González P. A. Vásquez Yerko 《The European Physical Journal C - Particles and Fields》2014,74(6):1-5
Following some recent unexpected hints of neutron production in high-voltage atmospheric discharges, we present a measurement of the neutron flux in plasma discharges in electrolytic cells. We use two different types of neutron detectors, polyallyl diglycol carbonate (PADC, aka CR-39) tracers and indium disks. At 95 % C.L. we provide an upper limit of 1.5 neutrons cm \(^{-2}\) s \(^{-1}\) for the thermal neutron flux at \({\approx } 5\) cm from the center of the cell. Allowing for a higher energy neutron component, the largest allowed flux is 64 neutrons cm \(^{-2}\) s \(^{-1}\) . This upper limit is two orders of magnitude smaller than the signal previously claimed in an electrolytic cell plasma discharge experiment. Furthermore the behavior of the CR-39 is discussed to point out possible sources of spurious signals. 相似文献