Quasinormal modes, shadow and greybody factors of 5D electrically charged Bardeen black holes

TL;DR

This paper investigates the quasinormal modes, shadow, and greybody factors of five-dimensional electrically charged Bardeen black holes, revealing how electric charge influences perturbation decay, oscillation rates, and spacetime oscillations.

Contribution

It provides the first detailed analysis of QNMs, shadow, and greybody factors for 5D charged Bardeen black holes, highlighting the effects of electric charge on these properties.

Findings

Electric charge slows decay of perturbations compared to Schwarzschild-Tangherlini black holes.

Scalar perturbations oscillate faster but damp more quickly than electromagnetic ones.

QNM frequencies decrease with increasing electric charge, affecting gravitational wave emission.

Abstract

We study quasinormal modes (QNMs) in 5D electrically charged Bardeen black holes spacetime by considering the scalar and electromagnetic field perturbations. The black holes spacetime is an exact solution of Einstein gravity coupled to nonlinear electrodynamics in five dimensions, which has nonsingular behavior. To calculate QNMs, we use the WKB approximation method up to sixth order. Due to the presence of electric charge $q_e > 0$, both the scalar and electromagnetic field perturbations decay more slowly when compared to the Schwarzschild-Tangherlini black holes. We discover that the scalar field perturbations oscillate more rapidly when compared to the electromagnetic field perturbations. In terms of damping, the scalar field perturbations damp more quickly. Graphically we show that the transmission (reflection) coefficients decrease (increase) with an increase in the magnitude of the electric charge $q_e$. The emission of gravitational waves allows spacetime to undergo damped oscillations due to the nonzero value of the imaginary part, which is always negative. The imaginary part of the QNMs frequencies is continuously decreasing with an increase in the magnitude of the electric charge $q_e$ for a given mode ($l,n$). A connection between the QNMs frequencies and the black hole shadow, as well as the geometric cross-section in the eikonal limit, is also described.