Black hole evaporation and semiclassical thin shell collapse

@article{Baccetti2019BlackHE,
  title={Black hole evaporation and semiclassical thin shell collapse},
  author={Valentina Baccetti and Sebastian Murk and Daniel R. Terno},
  journal={Physical Review D},
  year={2019}
}
In case of spherical symmetry the assumptions of finite-time formation of a trapped region and regularity of its boundary --- the apparent horizon --- are sufficient to identify the limiting form of the metric and the energy-momentum tensor in its vicinity. By comparison with the known results for quasi-static evaporation of black holes we complete the identification of their parameters. Consistency of the Einstein equations determines two possible types of higher-order terms in the energy… 

Figures from this paper

Self-consistent description of a spherically-symmetric gravitational collapse
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
Effective quantum dust collapse via surface matching
The fate of matter forming a black hole is still an open problem, although models of quantum gravity corrected black holes are available. In loop quantum gravity (LQG) models were presented, which
Properties of space-time in the vicinity of trapped regions
We study the near-horizon geometry in axisymmetric space-times. The general axisymmetric metrics have seven different parameters depending on three coordinates, and consistency analysis of the
Testing the nature of dark compact objects: a status report
Very compact objects probe extreme gravitational fields and may be the key to understand outstanding puzzles in fundamental physics. These include the nature of dark matter, the fate of spacetime
Alternative mechanism for black hole echoes
Hang Liu,1, 2, ∗ Wei-Liang Qian,3, 1, 4, † Yunqi Liu,1 Jian-Pin Wu,1 Bin Wang,1, 5, ‡ and Rui-Hong Yue1 1Center for Gravitation and Cosmology, College of Physical Science and Technology, Yangzhou
Universal properties of the near-horizon geometry
We derive universal properties of the near-horizon geometry of spherically symmetric black holes. These properties follow solely from the existence of an apparent horizon and its regularity. Only two
Bouncing compact objects. II. Effective theory of a pulsating Planck star
This article presents an effective quantum extension of the seminal Oppenheimer-Snyder (OS) collapse in which the singularity resolution is modeled using the effective dynamics of the spatially
Bouncing compact objects. Part I. Quantum extension of the Oppenheimer-Snyder collapse
This article proposes a generalization of the Oppenheimer-Snyder model which describes a bouncing compact object. The corrections responsible for the bounce are parameterized in a general way so as
Echoes from phantom wormholes
We study the time evolution of the test scalar and electromagnetic fields perturbations in configurations of phantom wormholes surrounded by dark energy with $\omega< -1$. We observe obvious signals
Geometry near the apparent horizon
Trapped regions bounded by horizons are the defining features of black holes. However, formation of a singularity-free apparent horizon in finite time of a distant observer is consistent only with
...
1
2
...

References

SHOWING 1-10 OF 62 REFERENCES
Role of evaporation in gravitational collapse
We investigate the possibility that quantum effects responsible for black hole radiation do not allow for hori- zon crossing of gravitationally collapsing matter in a finite time as seen by distant
Closed trapping horizons without singularity
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
Foliation dependence of black hole apparent horizons in spherical symmetry
Numerical studies of gravitational collapse to black holes make use of apparent horizons, which are intrinsically foliation dependent. We expose the problem and discuss possible solutions using the
Fate of gravitational collapse in semiclassical gravity
While the outcome of gravitational collapse in classical general relativity is unquestionably a black hole, up to now no full and complete semiclassical description of black hole formation has been
A Self-consistent Model of the Black Hole Evaporation
We construct a self-consistent model which describes a black hole from formation to evaporation including the backreaction from the Hawking radiation. In the case where a null shell collapses, at the
Nonlocal (but also nonsingular) physics at the last stages of gravitational collapse
We study the end stages of gravitational collapse of the thin shell of matter in ingoing Eddington-Finkelstein coordinates. We use the functional Schrodinger formalism to capture quantum effects in
Origin of Hawking radiation.
  • Hájícek
  • Physics
    Physical review. D, Particles and fields
  • 1987
TLDR
It seems that the Hawking effect is associated with themore rather than the event horizon, as an extrapolation of some properties of from a neighborhood of the Schwarzschild horizon to that of an apparent horizon forming in a collapse leads to the result that too much energy is radiated away already before the apparent horizon forms.
Radiation from collapsing shells, semiclassical backreaction, and black hole formation
We provide a detailed analysis of quantum field theory around a collapsing shell and discuss several conceptual issues related to the emission of radiation flux and formation of black holes. Explicit
Black hole evaporation: a paradigm
A paradigm describing black hole evaporation in non-perturbative quantum gravity is developed by combining two sets of detailed results: (i) resolution of the Schwarzschild singularity using quantum
Energy-momentum tensor and metric near the Schwarzschild sphere
Regularity of the horizon radius ${r}_{g}$ of a collapsing body constrains a limiting form of a spherically symmetric energy-momentum tensor near it. Its nonzero limit belongs to one of four classes
...
1
2
3
4
5
...