Cosmic Matter Flux May Turn Hawking Radiation Off

Abstract

An astrophysical (cosmological) black hole forming in a cosmological context will be subject to a flux of infalling matter and radiation, which will cause the outer apparent horizon (a marginal trapping surface) to be spacelike \cite{ellisetal14}. As a consequence the radiation emitted close to the apparent horizon no longer arrives at infinity with a diverging redshift. Standard calculations of the emission of Hawking radiation then indicate that no blackbody radiation is emitted to infinity by the black hole in these circumstances, hence there will also then be no black hole evaporation process due to emission of such radiation as long as the matter flux is significant. The essential adiabatic condition (eikonal approximation) for black hole radiation gives a strong limit to the black holes that can emit Hawking radiation. We give the mass range for the black holes that can radiate, according to their cosmological redshift, for the special case of the cosmic blackbody radiation (CBR) influx (which exists everywhere in the universe). At a very late stage of black hole formation when the CBR influx decays away, the black hole horizon becomes first a slowly evolving horizon and then an isolated horizon; at that stage, black hole radiation will start. This study suggests that the primordial black hole evaporation scenario should be revised to take these considerations into account.

To appear, GRG Journal

References in corpus (9)

• Numerical observation of Hawking radiation from acoustic black holes in atomic Bose-Einstein condensates
• Temporal contribution to gravitational WKB-like calculations
• Fate of gravitational collapse in semiclassical gravity
• Subtleties in the quasi-classical calculation of Hawking radiation
• Minimal conditions for the existence of a Hawking-like flux
• Hawking-like radiation from evolving black holes and compact horizonless objects
• Towards thermodynamics of universal horizons in Einstein-æther theory
• Evolution of Primordial Black Holes in a radiation and phantom energy environment
• Properties of Black Hole Radiation From Tunnelling

Cited by in corpus (7)

• Gravitational Analysis of Rotating Charged Black Hole-Like Solution in Einstein-Gauss-Bonnet Gravity
• Particle creation from the quantum stress tensor
• Constructing black hole entropy from gravitational collapse
• Radiation from Einstein-Gauss-Bonnet de Sitter Black Hole via Tunneling Process
• Logarithm Corrections and Thermodynamics for Horndeski gravity like Black Holes
• Evaporation and Antievaporation instabilities
• The generalized Lemaitre-Tolman-Bondi solutions with nonzero pressure in modeling the cosmological black holes