Solution of Dirac equation and greybody radiation around a regular Bardeen black hole surrounded by quintessence

Abstract

The exact solutions of the Dirac equation that describe a massive, non-charged particle with spin− 1 2 in the curved spacetime geometry of regular Bardeen black hole surrounded by quintessence (BBHSQ) are investigated. We first derive the Dirac equation in the BBHSQ background using a null tetrad in the Newman-Penrose formalism. Afterward, we separate the Dirac equation into ordinary differential equations for the radial and angular parts. The angular equations are solved exactly in terms of standard spherical harmonics. The radial part equations are transformed into a Schrödinger like differential wave equations with effective potentials. The effect of the quintessence on the regular Bardeen black hole is studied by understanding the physical behavior of the effective potentials. In addition, the potentials are plotted with changing the quintessence parameters, magnetic monopole charge parameter and the frequency of the particle in the physically acceptable regions. Finally, we study the greybody radiation of spin−0 particles from the BBHSQ.2

Greybody factor and perturbation of a Schwarzschild black hole with string clouds and quintessence

“…Studies have been conducted to compute the greybody factors, to examine the characteristic bosonic and fermionic quantum radiations, of different BH backgrounds. Such as the Dirac equation in regular Bardeen BH surrounded by quintessence [33], in four-dimensional non-Abelian charged Lifshitz black branes [34], in dRGT massive gravity coupled with nonlinear electrodynamics [35] and recently in Kerr-like black hole in Bumblebee gravity model [36].…”

Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model

“…Namely, Hawking radiation which is modified from the perfect black body spectrum is known as the GF [32,33]. There are different methods to compute the GF such as the WKB approximation [34,35], matching method [36,37], rigorous bound method [38], and analytical method for the various of spin fields [39][40][41][42][43][44]. Furthermore, in the framework of GR for the radiation of gravitational waves, the most important phase described in function of the proper oscillation frequencies of the black hole is called QNMs, which depend on the black hole parameters [46,47].…”

Physical Properties of Brane-World Black Hole Solutions via a Confining Potential

“…This phenomenon is known as greybody factor (GF) [27][28][29], which reveals important information about black holes and can be computed in various methods [30][31][32][33][34][35][36].…”