Measuring the Last Burst of Non-singular Black Holes

Vidotto, Francesca

doi:10.1007/s10701-018-0190-z

Cited by 7 publications

(7 citation statements)

References 47 publications

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“…While what we said above holds in the case of shortlived bounces of typical timescale τ (1) , more complex is the case of long-lived bounces with τ = τ (2) , for which several phenomenological studies have been performed in the literature [52,53,164,165]. In this case no relevant signal is expected up to this timescale while two distinct components are predicted as being associated to the typical size of the exploding object (infrared component) and to the typical energy of the universe at the moment of its formation (ultraviolet component).…”

Section: Burstsmentioning

confidence: 91%

“…For primordial black holes whose lifetime is of the order of the Hubble time, it was shown that the infrared component of the signal could get up to the GeV scale and be peaked in the MeV, while the ultraviolet part of the burst is expected to be in the TeV range [164,165]. If confirmed by more accurate modelling, this would place the search for the bursts associated to bouncing geometries within the realm of current high energy astrophysics experiments (provided that a sufficient number of primordial black holes is created in the early universe).…”

Section: Burstsmentioning

confidence: 99%

“…If confirmed by more accurate modelling, this would place the search for the bursts associated to bouncing geometries within the realm of current high energy astrophysics experiments (provided that a sufficient number of primordial black holes is created in the early universe). Furthermore, the fact that bursts further away in redshift would correspond to less massive and more primordial objects implies that their higher peak frequency would partially compensate their higher cosmological redshift [165]. This is a peculiar behaviour that might be used a a signature for this kind of signals and might help distinguish them from other, more standard, astrophysical emissions.…”

Section: Burstsmentioning

confidence: 99%

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Phenomenological aspects of black holes beyond general relativity

et al. 2018

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While singularities are inevitable in the classical theory of general relativity, it is commonly believed that they will not be present when quantum gravity effects are taken into account in a consistent framework. In particular, the structure of black holes should be modified in frameworks beyond general relativity that aim at regularizing singularities. Being agnostic on the nature of such theory, in this paper we classify the possible alternatives to classical black holes and provide a minimal set of phenomenological parameters that describe their characteristic features. The introduction of these parameters allows us to study, in a largely model-independent manner and taking into account all the relevant physics, the phenomenology associated with these quantummodified black holes. We perform an extensive analysis of different observational channels and obtain the most accurate characterization of the viable constraints that can be placed using current data. Aside from facilitating a critical revision of previous work, this analysis also allows us to highlight how different channels are capable of probing certain features but are oblivious to others, and pinpoint the theoretical aspects that should be addressed in order to strengthen these tests.

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Section: Burstsmentioning

confidence: 91%

Section: Burstsmentioning

confidence: 99%

Section: Burstsmentioning

confidence: 99%

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Phenomenological aspects of black holes beyond general relativity

et al. 2018

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“…For example, the smallest possible mass of a primordial black hole exploding today should be M ≃ 10 11 kg according to Ref. [14]. From Eq.…”

Section: Corpuscular Gravitymentioning

confidence: 99%

“…Several phenomenological studies concerning these loopy bouncing black holes have been carried out in the last few years (see e.g. [13,14] and references therein), with a natural focus on the final stages of evolution of primordial black holes. In these studies it was found that the mass of primordial black holes "exploding" today, after a time τ ∼ τ b from formation, should range from 10 11 kg to 10 20 kg [5,13].…”

Section: Introductionmentioning

confidence: 99%

The role of collapsed matter in the decay of black holes

Casadio

Giusti

2019

Physics Letters B

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We try to shed some light on the role of matter in the final stages of black hole evaporation from the fundamental frameworks of classicalization and the black-to-white hole bouncing scenario. Despite being based on very different grounds, these two approaches attempt at going beyond the background field method and treat black holes as fully quantum systems rather than considering quantum field theory on the corresponding classical manifolds. They also lead to the common prediction that the semiclassical description of black hole evaporation should break down and the system be disrupted by internal quantum pressure, but they both arrive at this conclusion neglecting the matter that formed the black hole. We instead estimate this pressure from the bootstrapped description of black holes, which allows us to express the total Arnowitt-Deser-Misner mass in terms of the baryonic mass still present inside the black hole. We conclude that, although these two scenarios provide qualitatively similar predictions for the final stages, the corpuscular model does not seem to suggest any sizeable deviation from the semiclassical time scale at which the disruption should occur, unlike the black-to-white hole bouncing scenario. This, in turn, makes the phenomenology of corpuscular black holes more subtle from an astrophysical perspective. * casadio@bo.infn.it † agiusti@bo.infn.it

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Black hole collapse and bounce in effective loop quantum gravity

Kelly

Santacruz

Wilson-Ewing

2020

Class. Quantum Grav.

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We derive effective equations with loop quantum gravity corrections for the Lemaître–Tolman–Bondi family of space-times, and use these to study quantum gravity effects in the Oppenheimer–Snyder collapse model. For this model, after the formation of a black hole with an apparent horizon, quantum gravity effects become important in the space-time region where the energy density and space-time curvature scalars become comparable to the Planck scale. These quantum gravity effects first stop the collapse of the dust matter field when its energy density reaches the Planck scale, and then cause the dust field to begin slowly expanding. Due to this continued expansion, the matter field will eventually extend beyond the apparent horizon, at which point the horizon disappears and there is no longer a black hole. There are no singularities anywhere in this space-time. In addition, in the limit that edge effects are neglected, we show that the dynamics for the interior of the star of uniform energy density follow the loop quantum cosmology effective Friedman equation for the spatially flat Friedman–Lemaître–Robertson–Walker space-time. Finally, we estimate the lifetime of the black hole, as measured by a distant observer, to be ∼(GM)2/ℓ Pl.

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Measuring the Last Burst of Non-singular Black Holes

Cited by 7 publications

References 47 publications

Phenomenological aspects of black holes beyond general relativity

Phenomenological aspects of black holes beyond general relativity

The role of collapsed matter in the decay of black holes

Black hole collapse and bounce in effective loop quantum gravity

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