Dynamical behavior and nonminimal derivative coupling scalar field of Reissner-Nordström black hole with a global monopole

Abstract

In this paper, we research the dynamical evolution and quasinormal modes of nonminimal derivative coupling scalar field in Reissner-Nordström spacetime with a global monopole. We also find that Hawking radiation behavior near the event horizon is similar to the scalar field case. In the whole spacetime, the conclusions show that weak coupling field will affect the dynamical behavior delicately, but the strong coupling constant η results in the deformation of dynamical evolution curve. When η > η c , the black hole system will not be stable. The break from the global monopole also intensely affect the dynamical behavior of this black hole spacetime. Furthermore, the break will promote the instability of the coupling field.

A matrix method for quasinormal modes: Kerr and Kerr–Sen black holes

“…Due to mathematical difficulties, an exact analytic solution is not always attainable. Therefore, semi-analytical approximate and numerical methods have been proposed to calculate the quasinormal frequency (QNF) [3][4][5][6][7], for example, the Pöschl-Teller potential method [8], continued fractions method [9,10], the Horowitz-Hubeny method (HH) for anti-de Sitter spacetime [11], the WKB approximation [12][13][14], the finite difference method [15][16][17][18][19][20] and the asymptotic iteration method [21][22][23][24] among others [25][26][27].In this letter, we make use of a matrix method [28] to calculate the scalar QNF's for rotating Kerr and Kerr-Sen black hole spacetimes. By using the method of separation of variables, the radial and angular parts of the linearized perturbation equation of the scalar fields are given by [29,30] (…”

Nonlinear electromagnetic quasinormal modes and Hawking radiation of a regular black hole with magnetic charge

“…This two-dimensional wave equation can be integrated numerically by using the finite difference method suggested in [29,30]. It can be discretized as…”

“…Then the corresponding potential function V (r ) can be determined, which is the key to the numerical computation of the QNM frequencies (QNFs). Numerical methods for calculation of the QNFs have been developed for several years, and now mainly consist of the time domain method [19][20][21], the expansion method [22,23], direct integration in the frequency domain [24], the WKB method [25][26][27][28], and the finite differential method [29,30]. Since the WKB scheme has been shown to be more accurate for both the real and the imaginary parts of the dominant QNMs with n ≤ l [31], we apply the WKB method to the QNF calculation and compare the results with the ones from the expansion method.…”

Dynamical Evolution of a Scalar Field Coupling to Einstein’s Tensor in Charged Braneworld Black Holes

“…This two-dimensional wave equation can be integrated numerically by using the finite difference method suggest in [28,35]. It can be discretized as…”

“…In this paper, we study a coupling field (scalar field coupling to Einstein's tensor) perturbation in braneworld black holes as scalar field is the simplest field that can couple to spacetime curvature, and the coupling term proposed as (κ 1 R μν + κ 2 g μν R)∂ μ ψ∂ ν ψ could lead to some meaningful physical results. Those are potentials to arise an ideal physics theory [28].…”