Abstract
Recently, there has been an interest in exploring black holes that are regular in the sense that the central curvature singularity is avoided. Here, we depict a method to obtain a regular black hole (RBH) spacetime from the unhindered gravitational collapse beginning with regular initial data of a spherically symmetric perfect fluid. In other words, we obtain the equilibrium (static) spacetime (ℳ,˜g) as a limiting case of the time-evolving (nonstationary) spacetime (ℳ,g). In the spirit of P. S. Joshi, D. Malafarina and R. Narayan, Class. Quantum Grav. 31 (2014) 015002, our description of gravitational collapse is implicit in nature in the sense that we do not describe the data at each time-slice. Rather, we impose a condition in terms of geometric and matter variables for the collapse to have an end-state that is devoid of incomplete geodesics but admits a marginally trapped surface (MTS). The admission of MTS causally disconnects two mutually exclusive regions ̂ℳ1 and ̂ℳ2⊂ℳ in the sense that ∀p∈̂ℳ2, the causal past of p does not intersect ̂ℳ1. While the classic Oppenheimer–Snyder collapse model necessarily produces a black hole with a Schwarzschild singularity at the center, we show here that there are classes of regular initial conditions for which the collapse gives rise to a RBH.
| You currently do not have access to the full text article. |
|---|
