Nonsingular black hole model as a possible end product of gravitational collapse

Mbonye, Manasse R.; Kazanas, Demosthenes

doi:10.1103/physrevd.72.024016

Cited by 53 publications

(69 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…eqs. (15) and (16)] and monotonically decreases outwards. The two integration constants Ω and J can then be determined by matching the interior and exterior solutions at the boundary r = r 2 .…”

Section: A Rotating Gravastar Modelmentioning

confidence: 99%

See 1 more Smart Citation

Ergoregion instability in rotating gravastars

2008

View full text Add to dashboard Cite

The ergoregion instability is known to affect very compact objects that rotate very rapidly and do not possess a horizon. We present here a detailed analysis on the relevance of the ergoregion instability for the viability of gravastars. Expanding on some recent results, we show that not all rotating gravastars are unstable. Rather, stable models can be constructed also with J/M 2 ∼ 1, where J and M are the angular momentum and mass of the gravastar, respectively. The genesis of gravastars is still highly speculative and fundamentally unclear if not dubious. Yet, their existence cannot be ruled out by invoking the ergoregion instability. For the same reason, not all ultra-compact astrophysical objects rotating with J/M 2 1 are to be considered necessarily black holes.

show abstract

Section: A Rotating Gravastar Modelmentioning

confidence: 99%

“…The equation of state used for p r (ρ) serves here only as a closure relation and is therefore chosen to be in the simplest possible form, namely a polynomial of the type [10,15] …”

Section: A Rotating Gravastar Modelmentioning

confidence: 99%

Ergoregion instability in rotating gravastars

2008

View full text Add to dashboard Cite

show abstract

“…Motivations for the exponential form of ρ may be found in [14], [36], where they chose n = 3, which simplifies some calculations. The values of the central density, ρ 0 , and of the fall-off constant, r 0 , may not be set arbitrarily, since one must make sure that the compactness does not exceed unity.…”

Section: Model 1: the Ansatz And An Inhomogeneous Density Distributionmentioning

confidence: 99%

“…The allowed values of σ are therefore the eigenvalues of (36). If all the eigenvalues are positive, then σ will always be real.…”

Section: Axial Stabilitymentioning

confidence: 99%

See 1 more Smart Citation

Gravastar solutions with continuous pressures and equation of state

DeBenedictis

Horvat

Ilijić

et al. 2006

Class. Quantum Grav.

156

136

View full text Add to dashboard Cite

show abstract

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

Brustein

Medved

2019

Fortschritte der Physik

View full text Add to dashboard Cite

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.

show abstract

Nonsingular black hole model as a possible end product of gravitational collapse

Cited by 53 publications

References 19 publications

Ergoregion instability in rotating gravastars

Ergoregion instability in rotating gravastars

Gravastar solutions with continuous pressures and equation of state

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

Contact Info

Product

Resources

About