Dark Energy and Condensate Stars: A Quantum Alternative to Classical Black Holes

Mazur, Paweł O.; Mottola, Emil

doi:10.1142/9789812704030_0064

Cited by 190 publications

(340 citation statements)

References 11 publications

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“…Furthermore, in the limit when R → R + s and R 0 → R − s , the Schwarzschild star turns out to be the non-singular gravitational condensate star or gravastar with a negative pressure interior and a surface tension at R s , proposed by Mazur and Mottola [60,61,62] as an alternative to black holes as the final state of gravitational collapse.…”

Section: Discussionmentioning

confidence: 99%

“…Additionally in the original Hawking [38] radiation derivation, the backward-in-time propagated mode seems to experience a large blueshift with energies larger than the Planck energy. It is expected that these highly 'blue-shifted' photons would leave a non-negligible 'imprint' on the spacetime geometry, making the approximation of fixed classical geometry background untenable [60,67]. Moreover, the arbitrarily large values of entropy at T H → 0 associated with the black hole as predicted by the Bekenstein [9] formula in the classical limit → 0 produces serious challenges to the foundations of quantum mechanics.…”

Section: List Ofmentioning

confidence: 99%

“…It is expected that these highly 'blue-shifted' photons would leave a non-negligible 'imprint' on the spacetime geometry, making the approximation of fixed classical geometry background untenable [60,67].…”

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

“…Some models have been introduced to alleviate some of the black hole paradoxes [10,22,96]. In particular, we concentrate in the gravastar (vacuum condensate gravitational star) model proposed by Mazur and Mottola [60,61,62].…”

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

“…This chapter is organized as follows: in section 2.1 we review the original gravastar model proposed by Mazur & Mottola [60,61,62]. In connection with gravastars, in section 2.2 we discuss the interior solution found by Schwarzschild [92] for a homo- Using the Komar formula [50], we show that the divergence in pressure is integrable producing a transverse pressure and a surface tension on a surface of discontinuous pressure.…”

Section: Introductionmentioning

confidence: 99%

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Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

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AcknowledgmentsI am grateful to the universe, for its harmony. The project is the study of integral and surface properties of slowly rotating homogeneous masses in the gravastar limit R → R s , where R s is the Schwarzschild radius. For this purpose we followed the perturbative method proposed by Hartle in 1967. In this model, the relativistic equations of structure for a slowly rotating star were derived at second order in the angular velocity Ω. An interesting, and educational, application of this model was investigated by Chandrasekhar and Miller. I am indebted to the Department of Physics andIn their approach, they solved numerically the structure equations of a homogeneous star (constant energy density) up to the Buchdahl bound (9/8)R s . Based on this work, our objective was to investigate the interesting region below the Buchdahl bound R s < R < (9/8)R s , which has not been studied previously in the literature.Our results were astonishing. We found that the surface properties and quadrupole mass moment approach the values corresponding to those of the Kerr metric when expanded at second order in angular momentum. This remarkable result provides a long sought solution to the problem of the source of rotation in the Kerr spacetime.iv

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Section: Discussionmentioning

confidence: 99%

Section: List Ofmentioning

confidence: 99%

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

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Quantum‐corrected Geometry of Horizon Vicinity

Park

2017

Fortschritte der Physik

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We study the deformation of the horizon-vicinity geometry caused by quantum gravitational effects. Departure from the semi-classical picture is noted, and the fact that the matter part of the action comes at a higher order in Newton's constant than does the Einstein-Hilbert term is crucial for the departure. The analysis leads to a Firewalltype energy measured by an infalling observer for which quantum generation of the cosmological constant is critical. The analysis seems to suggest that the Firewall should be a part of such deformation and that the information be stored both in the horizon-vicinity and asymptotic boundary region. We also examine the behavior near the cosmological horizon.

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Non‐Singular Black Holes Interiors Need Physics Beyond the Standard Model

Brustein

Medved

2019

Fortschritte der Physik

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The composition as well as the very existence of the interior of a Schwarzschild black hole (BH) remains at the forefront of interesting, open problems in fundamental physics. To address this issue, we turn to Hawking's "principle of ignorance", which says that, for an observer with limited information about a physical system, all descriptions that are consistent with known physics are equally valid. We compare three different observers who view the BH from the outside and agree on the external Schwarzschild geometry. First, the modernist, who accepts the classical BH as the final state of gravitational collapse, the singularity theorems that underlie this premise and the central singularity that the theorems predict. The modernist is willing to describe matter in terms of quantum fields in curved space but insists on (semi)classical gravity. Second is the skeptic, who wishes to evade any singular behavior by finding a loophole to the singularity theorems within the realm of classical general relativity (GR). The third is a postmodernist who similarly wants to circumvent the singularity theorems but is willing to invoke exotic quantum physics in the gravitational and/or matter sector to do so. The postmodern view suggests that the uncertainty principle can stabilize a classically singular BH in a similar manner to the stabilization of the classically unstable hydrogen atom: Strong quantum effects in the matter and gravitational sectors resolve the would-be singularity over horizon-sized length scales. The postmodern picture then requires a significant departure from (semi)classical gravity, as well as some exotic matter beyond the standard model of particle physics (SM). We find that only the postmodern framework is consistent with what is known so far about BH physics and conclude that a valid description of the BH interior needs matter beyond the SM and gravitational physics beyond (semi)classical GR.

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Dark Energy and Condensate Stars: A Quantum Alternative to Classical Black Holes

Cited by 190 publications

References 11 publications

Slowly rotating supercompact Schwarzschild stars

Slowly rotating supercompact Schwarzschild stars

Quantum‐corrected Geometry of Horizon Vicinity

Non‐Singular Black Holes Interiors Need Physics Beyond the Standard Model

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