Black hole in asymmetric cosmological bounce

Pérez, Daniela; Bergliaffa, Santiago Esteban Perez; Romero, Gustavo E.

doi:10.1002/asna.202113883

“…Once in the expanding phase, its size begins to increase proportionally to the square of the scale factor. This is not the case in the McVittie spacetime [12,13], where the black hole horizon merges with the cosmological horizon in the contracting phase before reaching the bounce. Such a solution, however, does not take into account the coupling of the black hole with the cosmic dynamics, as in the present work.…”

Section: Discussionmentioning

confidence: 95%

“…We showed that although the metric describes a black hole in the past of the bounce, the trapping horizon disappears close to it, when it merges with the cosmic horizon. This result remains valid even when the bounce is not symmetric [13]. If the black hole interacts with the cosmic fluid, however, the McVittie metric is not an adequate description of the situation because in such metric the central mass remains constant.…”

Section: Introductionmentioning

confidence: 84%

Survival of black holes through a cosmological bounce

Pérez,

Romero

2022

Preprint

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We analyze whether a black hole can exist and survive in a universe that goes through a cosmological bounce. To this end, we investigate a central inhomogeneity embedded in a bouncing cosmological background modeled by the comoving generalized McVittie metric. Contrary to other dynamical metrics available in the literature, this solution allows for the interaction of the central object with the cosmological fluid. We show that the horizons associated with this metric change with cosmic time because they are coupled to the cosmic evolution as the mass of the central object is always proportional to the scale factor: it decreases during contraction and increases during expansion phases. After a full analysis of the causal structure of this spacetime, we determine that a dynamical black hole persists during the contraction, bounce, and expansion of the universe. This result implies that there is a class of bouncing models that admits black holes at all cosmological epochs. If these models are correct approximation to the real universe, then black holes surviving a cosmic collapse could play some role in the subsequent expanding phase.

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“…Previous studies of black hole-cosmological bounces have either constructed initial data for black hole bouncing solutions [32], worked in a perturbative limit [33][34][35][36], or made use of analytic solutions (e.g. generalizations of the McVittie solutions [37][38][39]), that are limited by the fact that the metric evolution is prescribed ad-hoc, and from that the implied matter type and evolution is derived. The question of what happens to a black hole in a nonsingular cosmological bounce is particular salient for several reasons.…”

Section: Introductionmentioning

confidence: 99%

Evolution of black holes through a nonsingular cosmological bounce

Corman,

East,

Ripley

2022

Preprint

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We study the classical dynamics of black holes during a nonsingular cosmological bounce. Taking a simple model of a nonsingular bouncing cosmology driven by the combination of a ghost and ordinary scalar field, we use nonlinear evolutions of the Einstein equations to follow rotating and non-rotating black holes of different sizes through the bounce. The violation of the null energy condition allows for a shrinking black hole event horizon and we find that for sufficiently large black holes (relative to the minimum Hubble radius) the black hole apparent horizon can disappear during the contraction phase. Despite this, we show that most of the local cosmological evolution remains largely unaffected by the presence of the black hole. We find that, independently of the black hole's initial mass, the black hole's event horizon persists throughout the bounce, and the late time dynamics consists of an expanding universe with a black hole of mass comparable to its initial value.

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“…Previous studies of black hole-cosmological bounces have either constructed initial data for black hole bouncing solutions [34], worked in a perturbative limit [35][36][37][38], or made use of analytic solutions (e.g. generalizations of the McVittie solutions [39][40][41]), that are limited by the fact that the metric evolution is prescribed ad-hoc, and from that the implied matter type and evolution is derived. The question of what happens to a black hole in a nonsingular cosmological bounce is particular salient for several reasons.…”

Section: Introductionmentioning

confidence: 99%

Evolution of black holes through a nonsingular cosmological bounce

Corman

¹

,

East

²

,

Ripley

³

2022

J. Cosmol. Astropart. Phys.

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We study the classical dynamics of black holes during a nonsingular cosmological bounce. Taking a simple model of a nonsingular bouncing cosmology driven by the combination of a ghost and ordinary scalar field, we use nonlinear evolutions of the Einstein equations to follow rotating and non-rotating black holes of different sizes through the bounce. The violation of the null energy condition allows for a shrinking black hole event horizon and we find that for sufficiently large black holes (relative to the minimum Hubble radius) the black hole apparent horizon can disappear during the contraction phase. Despite this, we show that most of the local cosmological evolution remains largely unaffected by the presence of the black hole. We find that, independently of the black hole's initial mass, the black hole's event horizon persists throughout the bounce, and the late time dynamics consists of an expanding universe with a black hole of mass comparable to its initial value.

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Black hole in asymmetric cosmological bounce

Cited by 4 publications

References 22 publications

Survival of black holes through a cosmological bounce

Survival of black holes through a cosmological bounce

Evolution of black holes through a nonsingular cosmological bounce

Evolution of black holes through a nonsingular cosmological bounce

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