Surrounded Bonnor–Vaidya solution by cosmological fields

Abstract

In the present work, we generalize our previous work (Heydarzade and Darabi in arXiv:1710.04485, 2018 on the surrounded Vaidya solution by cosmological fields to the case of Bonnor-Vaidya charged solution. In this regard, we construct a solution for the classical description of the evaporating-accreting charged Bonnor-Vaidya black holes in the generic dynamical backgrounds. We address some interesting features of these solutions and classify them according to their behaviors under imposing the positive energy condition. Also, we analyze the timelike geodesics associated with the obtained solutions and show that some new correction terms arise in comparison to the case of standard Schwarzschild black hole. Then, we explore all these features for each of the cosmological backgrounds of dust, radiation, quintessence and cosmological constant-like fields in more detail.

Thin shell collapse in Kiselev geometry

“…In the latter case, we have shown that the equation of state parameter must be positive because of the requirement that the shell is timelike and the energy density is positive. Invoking Barrabès-Israel junction conditions we found out that stationary BH solutions can be found from equations (44) and (45) where we have concluded that the normalized shell mass should satisfy M < 1/2. Stability of these solutions have been examined numerically and it is shown that for ω < 1/3, there exists stable BH solutions with negative shell mass which is unbounded from below.…”

“…in which Θ is the step function. This is a particular case of Vaidya generalization of Kiselev metric [45] defined by m(v) = mΘ(v − v 0 ) and c(v) = cΘ(v − v 0 ). Moreover, the above mentioned metric for ω = −1 is a special case of a large family of dynamical BH introduced in [46].…”

“…To obtain some sequences of stable stationary regular BHs with fixed values of m and ω, the shell mass, M(R), is found from equation (44). Once M(R) is determined, the parameter c can be obtained from (45). As it was mentioned before, for ω < 1/3, there are stable BH solutions with both positive and negative shell mass.…”

Gravitational wave pulse and memory effects for hairy Kiselev black hole and its analogy with Bondi–Sachs formalism

“…This allows for a wide range of possibilities, including quintessence, cosmological constant, radiation, and dust-like fields. Furthermore, the dynamical Vaidya-type solutions have also been generalized based on this initial solution [21][22][23]. These generalizations are well-founded due to the non-isolated nature of real-world black holes and their existence in non-vacuum backgrounds.…”

Conformal symmetries in generalised Vaidya spacetimes

“…Detailed study of continual gravitational collapse of these spacetimes in the context of the Cosmic Censorship Conjecture were done in [23,24]. In the geometrical context, gravitational collapse has been considered in Lovelock gravity theory [25], black holes in dynamical cosmology backgrounds [26] and in electromagnetic fluids [27]. The influence of dust, radiation, quintessence and the cosmological constant are included in these studies.…”