# Formation and evaporation of nonsingular black holes.

@article{Hayward2006FormationAE, title={Formation and evaporation of nonsingular black holes.}, author={Sean A. Hayward}, journal={Physical review letters}, year={2006}, volume={96 3}, pages={ 031103 } }

Regular (nonsingular) space-times are given that describe the formation of a (locally defined) black hole from an initial vacuum region, its quiescence as a static region, and its subsequent evaporation to a vacuum region. The static region is Bardeen-like, supported by finite density and pressures, vanishing rapidly at large radius and behaving as a cosmological constant at small radius. The dynamic regions are Vaidya-like, with ingoing radiation of positive-energy flux during collapse and…

## 491 Citations

Models for the nonsingular transition of an evaporating black hole into a white hole.

- Physics
- 2018

There have been recent suggestions that the r = 0 singularity of a spherically symmetric evaporating black hole can be circumvented by a quantum transition to a white hole, which eventually releases…

Modelling the evaporation of nonsingular black holes

- Physics
- 2014

We present a model for studying the formation and evaporation of non-singular (quantum corrected) black holes. The model is based on a generalized form of the dimensionally reduced, spherically…

Model for nonsingular black hole collapse and evaporation

- Physics
- 2010

We study the formation of a black hole and its subsequent evaporation in a model employing a minisuperspace approach to loop quantum gravity. In previous work the static solution was obtained and…

Trapping horizon and negative energy

- PhysicsJournal of High Energy Physics
- 2019

A bstractAssuming spherical symmetry and the semi-classical Einstein equation, we prove that, for the observers on top of the trapping horizon, the vacuum energy-momentum tensor is always that of an…

Self-consistent description of a spherically-symmetric gravitational collapse

- PhysicsPhysical Review D
- 2019

In spherical symmetry, the total energy-momentum tensor near the apparent horizon is identified up to a single function of time from two assumptions: a trapped region forms at a finite time of a…

Can a false vacuum bubble remove the singularity inside a black hole?

- Physics
- 2019

We investigate a regular black hole model with a de Sitter-like core at its center. This type of a black hole model with a false vacuum core was introduced with the hope of singularity-resolution and…

Closed trapping horizons without singularity

- PhysicsPhysical Review D
- 2018

In gravitational collapse leading to black hole formation, trapping horizons typically develop inside the contracting matter. Classically, an ingoing trapping horizon moves toward the center where it…

SPHERICALLY SYMMETRIC TRAPPING HORIZONS, THE MISNER SHARP MASS AND BLACK HOLE EVAPORATION

- Physics
- 2009

We discuss some of the issues relating to information loss and black hole thermodynamics in the light of recent work on local black hole horizons. Understood in terms of pure states evolving into…

Global Causal Structure of a Transient Black Object

- Physics
- 2011

A singularity-free and spherically symmetric transient black object whose center remains always timelike, yet directly manifests a trapped region, has been constructed and numerically implemented.…

## References

SHOWING 1-10 OF 64 REFERENCES

Energy conservation for dynamical black holes.

- PhysicsPhysical review letters
- 2004

An energy conservation law is described, expressing the increase in mass-energy of a general black hole in terms of the energy densities of the infalling matter and gravitational radiation. This…

Nonsingular black hole model as a possible end product of gravitational collapse

- Physics
- 2005

In this paper we present a nonsingular black hole model as a possible end-product of gravitational collapse. The depicted spacetime which is type [II,(II)], by Petrov classification, is an exact…

Stellar collapse without singularities

- Physics
- 1983

For the singularity theorems of Hawking and Penrose to hold, the stress-energy tensor of matter must satisfy certain restrictions. A model is developed representing the interior of a collapsing,…

Energy and entropy conservation for dynamical black holes

- Physics
- 2004

The Ashtekar-Krishnan energy-balance law for dynamical horizons, expressing the increase in mass-energy of a general black hole in terms of the infalling matter and gravitational radiation, is…

General laws of black-hole dynamics.

- GeologyPhysical review. D, Particles and fields
- 1994

The future outer trapping horizon provides the definition of a black hole, and general ``laws of black-hole dynamics'' derived.

Dynamical Horizons and their Properties

- Physics
- 2003

A detailed description of how black holes grow in full, non-linear general relativity is presented. The starting point is the notion of dynamical horizons. Expressions of fluxes of energy and angular…

Local existence of dynamical and trapping horizons.

- MathematicsPhysical review letters
- 2005

Given a spacelike foliation of a spacetime and a marginally outer trapped surface S on some initial leaf, we prove that under a suitable stability condition S is contained in "horizon" i.e., a smooth…

Black holes as possible sources of closed and semiclosed worlds.

- PhysicsPhysical review. D, Particles and fields
- 1990

It is shown that instead of the singularity the closed world can be formed inside the black hole and it is argued that this property of this model may also be valid in a more general case provided the gravitation theory is asymptotically free and the limiting curvature exists.

Global structure of a black hole cosmos and its extremes

- Physics
- 1994

We analyze the global structure of a family of Einstein-Maxwell solutions parametrized by mass, charge and cosmological constant. In a qualitative classification there are: (i) generic black-hole…

Stability of the Schwarzschild-de Sitter model.

- PhysicsPhysical review. D, Particles and fields
- 1990

It is shown that the uniform configuration considered by Frolov, Markov, and Mukhanov is a stable configuration (in the sense that, when perturbed, the three-cylinder does not tend to shrink down to a point as a cone) and does not require fine-tuning.