Observation of Incipient Black Holes and the Information Loss Problem

  title={Observation of Incipient Black Holes and the Information Loss Problem},
  author={Tanmay Vachaspati and Dejan Stojkovi{\'c} and Lawrence Krauss},
  journal={Physical Review D},
We study the formation of black holes by spherical domain wall collapse as seen by an asymptotic observer, using the functional Schrodinger formalism. To explore what signals such observers will see, we study radiation of a scalar quantum field in the collapsing domain wall background. The total energy flux radiated diverges when backreaction of the radiation on the collapsing wall is ignored, and the domain wall is seen by the asymptotic observer to evaporate by nonthermal "pre-Hawking… 
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
The Absence of Horizon in Black-Hole Formation
With the back-reaction of Hawking radiation taken into consideration, the work of Kawai, Matsuo and Yokokura [1] has shown that, under a few assumptions, the collapse of matter does not lead to event
Properties of Black Hole Radiation From Tunnelling
We consider the spacetime associated with the evaporation of a black hole by quantum mechanical tunnelling events. It is shown that the surface through which tunnelling occurs is distinct from the
Pre-Hawking radiation from a collapsing shell
We investigate the effect of induced massive radiation given off during the time of collapse of a massive spherically symmetric domain wall in the context of the functional Schrodinger formalism.
Formation of the Hayward black hole from a collapsing shell
We consider a collapsing shell of matter to form the Hayward black hole and investigate semi-classically quantum radiation from the shell. Using the Israel's formulation, we obtain the mass relation
Asymptotic black holes
Following earlier works on the KMY model of black-hole formation and evaporation, we construct the metric for a matter sphere in gravitational collapse, with the back-reaction of pre-Hawking
Black hole evaporation and semiclassical thin shell collapse
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
Pre-Hawking radiation may allow for reconstruction of the mass distribution of the collapsing object
Abstract Hawking radiation explicitly depends only on the black hole's total mass, charge and angular momentum. It is therefore generally believed that one cannot reconstruct the information about
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
Interior of Black Holes and Information Recovery
We analyze time evolution of a spherically symmetric collapsing matter from a point of view that black holes evaporate by nature. We first consider a spherical thin shell that falls in the metric of


Hawking-like radiation does not require a trapped region.
It is shown that, in order to obtain a stationary and Planckian emission of quasiparticles, it is not necessary to create a trapped region in the acoustic spacetime, and it is sufficient to set up a dynamically changing flow asymptotically approaching a sonic regime with sufficient rapidity in laboratory time.
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
Information loss in black holes
The question of whether information is lost in black holes is investigated using Euclidean path integrals. The formation and evaporation of black holes is regarded as a scattering problem with all
Evanescent black holes.
A renormalizable theory of quantum gravity coupled to a dilaton and conformal matter in two spacetime dimensions is analyzed and suggests that the collapsing matter radiates away all of its energy before an event horizon has a chance to form, and black holes disappear from the quantum-mechanical spectrum.
The Mechanism of blackbody radiation from the incipient black hole
On the basis of the phenomenon of zero-point energy an account is given of the mechanism of the emission of blackbody radiation from an incipient (about-to-be-formed) black hole, which results from
Origin of Hawking radiation.
  • Hájícek
  • Physics, Medicine
    Physical review. D, Particles and fields
  • 1987
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.
Hawking radiation and thin shells
The properties of quantized scalar and Dirac fields around a collapsing thin shell are discussed and the Hawking radiation exhibited. The radiation is seen to be a result of the collapse process
Energy-momentum tensor near an evaporating black hole
We calculate the vacuum expectation value, T/sub ..mu nu../, of the energy--momentum tensor of a massless scalar field in a general two-dimensional spacetime and evaluate it in a two-dimensional
Gravitational collapse of a radiating shell
We study the collapse of a self-gravitating and radiating shell. Matter constituting the shell is quantized and the construction is viewed as a semiclassical model of possible black hole formation.
Particle creation by black holes
AbstractIn the classical theory black holes can only absorb and not emit particles. However it is shown that quantum mechanical effects cause black holes to create and emit particles as if they were