Information loss problem and a ‘black hole’ model with a closed apparent horizon

By Valeri P. Frolov. 2014

154 citations recorded by the source corpus.

A bstractIn a classical description the spacetime curvature inside a black hole infinitely grows. In the domain where it reaches the Planckian value and exceeds it the Einstein equations should be modified. In the absence of reliable theory of quantum gravity it is instructive to consider simplified models. We assume that a spacetime curvature is limited by some value (of the order of the Planckian one). We use modified Vaidya metric, proposed by Hayward, to describe the black hole evaporation process. In such a spacetime the curvature near r = 0 remains finite, it does not have an event horizon and its apparent horizon is closed. If the initial mass of such a ‘black hole’ is much larger than the Planckian one its properties (as seen by an external observer) are practically the same as properties of the ‘standard’ black hole with the event horizon. We study outgoing null rays in the vicinity of the outer apparent horizon and introduce a notion of a quasi-horizon. We demonstrate that particles, trapped inside a ‘black hole’ during the evaporation process, finally may return to external space after the evaporation is completed. We also demonstrate that such quanta would have very large blue-shift. The absence of the event horizon makes it possible restoration of the unitarity in evaporating black holes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/39700f718466e9411e4e74f33e0b807abcad1266

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

In Statistical and Nonlinear Physics

Citations in the corpus

Regular Black Holes with Asymptotically Minkowski Cores (2019, background): “[3–7]) regular black holes, but also the Mazur–Mottola gravastars [8–16], and Dymnikova’s models [17–21].”
Black-bounce to traversable wormhole (2018, background): “This metric does not correspond to a traditional regular black hole such as the Bardeen, Bergmann–Roman, Frolov, or Hayward geometries [1–11].”
On the viability of regular black holes (2018, background): “ciple [13]). In principle, it is not guaranteed that a complete quantum gravity theory allows for such an eective description, so that this is just a working assumption. As discussed for instance in [9,14], regular black holes provide an in principle complete and self-consistent picture for the evap”