Asymptotic horizon formation, spacetime stretching, and causality

Barceló, Carlos; Boyanov, Valentin; Carballo-Rubio, Raúl; Garay, Luis J.

doi:10.1103/physrevd.102.045001

Cited by 4 publications

(2 citation statements)

References 14 publications

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“…To see how the surface gravity diverges, first we need to define this quantity more precisely. Following the procedure from our previous work [21], we will use the generalised redshift function F(v, r), which goes on the right-hand side of the equation for outgoing null radial geodesics,…”

Section: Oppenheimer-snyder Collapsementioning

confidence: 99%

Black hole inner horizon evaporation in semiclassical gravity

Barceló

Boyanov

Carballo-Rubio³

et al. 2021

Class. Quantum Grav.

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In this work we analyse the backreaction of a quantum field on a spherically symmetric black hole geometry with an inner horizon, i.e. an internal boundary of the trapped region. We start with a black hole background with an inner horizon which remains static after its formation. We quantise a massless scalar field on it and calculate its renormalised stress-energy tensor in the Polyakov approximation. We use this tensor as a source of perturbation on top of the background spacetime. We find that the inner horizon has a tendency to evaporate outward much more quickly than the outer one evaporates inward through the Hawking effect. This suggests a revised picture of a semiclassically selfconsistent evaporation in which the dominant dynamical effect comes from the inner horizon, the cause of which can be seen as an interplay between the wellknown unstable nature of this horizon and a locally negative energy contribution from the quantum vacuum. We also look at backreaction on backgrounds which resemble gravitational collapse, where the inner horizon moves towards the origin. There we find that, depending on the nature of the background dynamics, horizon-related semiclassical effects can become dominant and invert the collapse.

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Section: Oppenheimer-snyder Collapsementioning

confidence: 99%

Black hole inner horizon evaporation in semiclassical gravity

Barceló

Boyanov

Carballo-Rubio³

et al. 2021

Class. Quantum Grav.

Self Cite

View full text Add to dashboard Cite

show abstract

“…To see how the surface gravity diverges, first we need to define this quantity more precisely. Following the procedure from our previous work [17], we will use the generalised redshift function F (v, r), which goes on the right-hand side of the equation for outgoing null radial geodesics,…”

Section: Oppenheimer-snyder Collapsementioning

confidence: 99%

Black hole inner horizon evaporation in semiclassical gravity

Barceló,

Boyanov,

Carballo-Rubio

et al. 2020

Preprint

Self Cite

View full text Add to dashboard Cite

In this work we analyse the backreaction of a quantum field on a spherically symmetric black hole geometry with an inner horizon, i.e. an internal boundary of the trapped region. We start with a black hole background with an inner horizon which remains static after its formation. We quantise a massless scalar field on it and calculate its renormalised stress-energy tensor in the Polyakov approximation. We use this tensor as a source of perturbation on top of the background spacetime. We find that the inner horizon has a tendency to evaporate outward much more quickly than the outer one evaporates inward through the Hawking effect. This suggests a revised picture of a semiclassically self-consistent evaporation in which the dominant dynamical effect comes from the inner horizon. We also look at backreaction on backgrounds which resemble gravitational collapse, where the inner horizon moves toward the origin. There we find that, depending on the nature of the background dynamics, horizon-related semiclassical effects can become dominant and invert the collapse.

show abstract