Pre-Hawking radiation cannot prevent the formation of apparent horizon

Abstract

As an attempt to solve the black hole information loss paradox, recently there has been the suggestion that, due to semi-classical effects, a pre-Hawking radiation must exist during the gravitational collapse of matter, which in turn prevents the apparent horizon from forming. Assuming the pre-Hawking radiation does exist, here we argue the opposite. First we note that the stress energy tensor near the horizon for the pre-Hawking radiation is far too small to do anything to the motion of a collapsing shell. Thus the shell will always cross the apparent horizon within a finite proper time. Moreovall, the amount of energy that can be radiated must be less than half of the total initial energy (if the particle starts at rest at infinity) before the shell becomes a null shell and cannot radiate any more without becoming tachyonic. We conclude that for any gravitational collapsing process within Einstein gravity and semi-classical quantum field theory, the formation of the apparent horizon is inevitable. Pre-Hawking radiation is therefore not a valid solution to the information paradox.

arXiv comment6 pages, 2 figures

References in corpus (10)

• Minimal conditions for the existence of a Hawking-like flux
• Hawking-like radiation from evolving black holes and compact horizonless objects
• A Self-consistent Model of the Black Hole Evaporation
• Hawking-like radiation does not require a trapped region
• Interior of Black Holes and Information Recovery
• Radiation from collapsing shells, semiclassical backreaction and black hole formation
• The Absence of Horizon in Black-Hole Formation
• Comment on Self-Consistent Model of Black Hole Formation and Evaporation
• Do event horizons exist?
• Model for Quantum Effects in Stellar Collapse

Cited by in corpus (23)

• Testing the nature of dark compact objects: a status report
• Phenomenological aspects of black holes beyond general relativity
• Stability of rotating scalar boson stars with nonlinear interactions
• Role of evaporation in gravitational collapse
• Quantum fields during black hole formation: How good an approximation is the Unruh state?
• Black hole evaporation and semiclassical thin shell collapse
• Effective black-to-white hole bounces: The cost of surgery
• Giant Tortoise Coordinate
• Pandora's box lid: geometry near the apparent horizon
• Avoidance of singularity during the gravitational collapse with string T-duality effects
• Transition to light-like trajectories in thin shell dynamics
• Particle creation in gravitational collapse to a horizonless compact object
• Understanding black hole evaporation using explicitly computed Penrose diagrams
• Can a false vacuum bubble remove the singularity inside a black hole?
• Burst particle creation in gravitational collapse to a horizonless compact object
• Quantum gravitational wave function for the interior of a black hole and the generalized uncertainty principle
• How Anti-de Sitter Black Holes Reach Thermal Equilibrium
• Quantum vacuum effects on the formation of black holes
• Unveiling horizons in quantum critical collapse
• Computation of the semiclassical outflux emerging from a collapsing spherical null shell
• Tunneling from the past horizon
• Black holes and their horizons in semiclassical and modified theories of gravity
• Black Holes as a Gateway to the Quantum: Classical and Semi-Classical Explorations