Abstract

In this paper we propose a class of non-stationary solutions of Einstein’s field equations describing an embedded Vaidya-de Sitter solution with a cosmological variable function Λ(u). Vaidya-de Sitter solution is interpreted as the radiating Vaidya black hole which is embedded into the non-stationary de Sitter space with variable Λ(u). The energymomentum tensor of the Vaidya-de Sitter black hole may be expressed as the sum of the energy-momentum tensor of the Vaidya null fluid and that of the non-stationary de Sitter field, and satisfies the energy conservation law. We also find that the equation of state parameter w= p/ρ = -1 of the non-stationary de Sitter solution holds true in the embedded Vaidya-de Sitter solution. It is also found that the space-time geometry of non-stationary Vaidya-de Sitter solution with variable Λ(u) is type D in the Petrov classification of space-times. The surface gravity, temperature and entropy of the space-time on the cosmological black hole horizon are discussed.

Highlights

  • The Vaidya solution having a variable mass m(u) with retarded time u is a non-stationary generalization of Schwarzschild black hole of constant mass m [1]

  • The Schwarzschild-de Sitter solution is interpreted as a black hole in an asymptotically de Sitter space with non-zero cosmological constant Λ [2]

  • We propose an exact solution describing the Vaidya-de Sitter solution with a non-stationary variable Λ(u), which may be treated as the non-stationary Vaidya-de Sitter black hole or the Vaidya black hole on the non-stationary de Sitter background with variable Λ(u)

Read more

Summary

Introduction

The Vaidya solution having a variable mass m(u) with retarded time u is a non-stationary generalization of Schwarzschild black hole of constant mass m [1]. The aim of this paper is to propose an exact solution of Einstein’s field equations describing Vaidya black hole embedded into the non-stationary de Sitter space to obtain Vaidya-de Sitter black hole with variable Λ(u). This non-stationary part of the energy-momentum tensor (1.2) contributes the nature of null matter field present in (1.1) whose energymomentum tensor Ta bNS has zero trace and will vanish when r → 0. With the negative pressure p in (1.6) This shows the fact that the non-stationary de Sitter solution (1.1) is in agreement with the cosmological constant (Λ) de Sitter model possessing the equation of state w = −1 in the dark energy scenario [9,10,11], when Λ(u) takes a constant value Λ. Embedded black holes can avoid the direct formation of negative mass naked singularities during Hawking’s black hole evaporation process [12]

Vaidya in Non-Stationary de Sitter Space
Cpqrs p mq mr ns m u r 3
Conclusions
Full Text
Paper version not known

Talk to us

Join us for a 30 min session where you can share your feedback and ask us any queries you have

Schedule a call

Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.