Quasinormal modes of a Schwarzschild black hole immersed in an electromagnetic universe

Abstract

We study the quasinormal modes (QNMs) of the Schwarzschild black hole immersed in an electromagnetic (em) universe. The immersed Schwarzschild black hole (ISBH) is originated from the metric of colliding em waves with double polarization [Class. Quantum Grav. 12, 3013 (1995)]. The perturbation equations of the scalar fields for the ISBH geometry are written in the form of separable equations. We show that these equations can be transformed to the confluent Heun's equations, for which we are able to use the known techniques to perform the analytical quasinormal (QNM) analysis of the solutions. Furthermore, we employ numerical methods [Mashhoon and 6 th -order Wentzel-Kramers-Brillouin (WKB)] to derive the QNMs. The results obtained are discussed and depicted with the appropriate plots.

Dirac Equation on the Kerr–Newman Spacetime and Heun Functions

“…For the asymptotic behavior at infinity, one may use formula (38) and expression (43) turns into the simplified form:…”

“…By imposing the necessary condition for a polynomial form of the Heun confluent functions [18,19], we obtain the resonant frequencies, which are of crucial importance for getting information on the black holes interacting with different quantum fields [24]. In the last years, the Heun functions in either their general or confluent forms have been obtained by many authors, for example, [25][26][27][28][29][30][31][32][33][34][35][36][37][38][39][40] and the references therein.…”

Echoes of charged black-bounce spacetimes

“…On the other hand, as the characteristic sound of black holes, the quasinormal models (QNMs) are dominantly governed by the spacetimes in the vicinity of the horizon. It is well known that once a black hole is perturbed [11], there are three stages that are responsible for the perturbations evolution in time. The first one is a relatively short period of initial outburst of radiation, the second one is a usually long period of damping proper oscillations which dominated by the QNM, and the third one is the power-law tail.…”

Quasinormal Modes of Extended Gravity Black Holes

“…The theory of QNMs of compact objects from both the mathematical and astrophysical points of view was considerably discussed in the literature (see for example [2,3] and references therein). Some researchers have generalized the effects of dark matter and dark energy on QNMs and some have developed the investigation of QNMs of various type of black holes in lower/higher dimensional spacetimes [4][5][6][7][8][9][10][11][12][13][14]. It is also worth noting that QNMs of BHs in AdS space (when the black hole is immersed in an expanding universe) have been recently studied [15].…”