Double-bounce domain wall in Einstein–Yang–Mills-Scalar black holes

Abstract

We find Einstein-Yang-Mills (EYM) black hole solutions endowed with massless scalar hair in the presence of a potential V (φ) as function of the scalar field φ. Choosing V (φ) = constant (or zero) sets the scalar field to vanish leaving us with the EYM black holes. Our class of black hole solutions is new so that they do not asymptotically go in general to any known limits. A particular case is given, however, which admits an asymptotically anti-de Sitter limit in 6-dimensional spacetime. The role of the potential V (φ) in making double bounces (i.e. both a minimum and maximum radii) on a domain wall universe is highlighted.

Modified gravity in three dimensional metric-affine scenarios

“…where r 2 (x) andr 2 (x) are, in general, functions of the coordinate x, while ξ(x) and A(x) are functions to be determined by solving the field equations and the functions B(x) and C(x) follow by consistency from the relations (9). Inserting (16) into (10), and taking into account the matter symmetry, T t t = T x x , from the combination R t t = R x x it follows that ξ(x) =constant. Through some redefinitions, and without loss of generality, the line element (16) can be rewritten as…”

“…Inserting (16) into (10), and taking into account the matter symmetry, T t t = T x x , from the combination R t t = R x x it follows that ξ(x) =constant. Through some redefinitions, and without loss of generality, the line element (16) can be rewritten as…”

“…In three space-time dimensions, regular black hole solutions have been obtained as generalizations of the Bardeen solution [13]. Other three dimensional spacetimes include wormhole solutions in nonlinear electrodynamics [14,15], charged shells scenarios [16], black holes with dilaton fields [17], magnetic solutions [18], and further extensions of the BTZ solution [19].…”

Quantum gravity effect on the Hawking radiation of charged rotating BTZ black hole

“…The coupling nonlinear electrodynamics theory to Einstein gravitation theory was firstly worked out by Hoffmann [69]. Furthermore, after Bardeen firstly introduced a regular black hole solution in the context of Einstein-nonlinear electrodynamics theory [70], the interest on this theory has increased and new black hole solutions found in 3+1 dimensional as well as 2+1 dimensional [71,72,73,74,75,76].…”

Stability of spherically symmetric timelike thin-shells in general relativity with a variable equation-of-state

“…Stability of charged thin-shells was considered in [15] and its collapse in isotropic coordinates was investigated in [16]. In [17] charge screening by thin-shells in a 2 + 1−dimensional regular black hole has been studied while the thermodynamics, entropy, and stability of thin-shells in 2 + 1−dimensional flat spacetimes have been given in [18] and [19]. Recently in [20] the stability of thin-shell interfaces inside compact stars has been studied by Pereira et al which is very interesting as they consider a compact star with the core and the crust with different energy momentum tensors and consequently with different metric tensors.…”