Gravitational collapse of quantum matter

Tippett, Benjamin K.; Husain, Viqar

doi:10.1103/physrevd.84.104031

Cited by 22 publications

(20 citation statements)

References 23 publications

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“…The mass loss obtained therein, was characterised by a reduction of the energy density and mass function towards the centre of the star, which leaded to an outward energy flux from the interior region and reaching the distant observer. In addition, in the cases in which one or two horizons form, the resulting exterior geometry corresponds to an exotic nonsingular black hole which is different from the Schwarzschild spacetime [15,21].…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…Furthermore, some novel features such as evaporation of horizons in the presence of quantum gravity effects were studied in Refs. [14,21]. In addition, it was shown in the Ref.…”

Section: Introductionmentioning

confidence: 97%

“…(4.5) represents a non singular, exotic black hole geometry. Notice that, the effective exterior function F eff = (1 − 2GM /R) in the classical limit, where ρ cr → ∞, tends to F = 1 − 2GC/R 4 , which represents a classical singular black hole geometry [21]. In addition, as we expected, in the presence of a nonzero matter pressure (of the massless scalar field) at the boundary, the (homogeneous) interior spacetime is not matched with an empty (inhomogeneous) Schwarzschild exterior [15].…”

Section: Semiclassical Outcomes Of the Collapsementioning

confidence: 99%

“…Therein, different fields, such as the standard scalar [14,15,21] or the tachyon [16,22], have been considered to play the role of the collapsing matter source. By employing the quantum gravity effects (such as the inverse triad correction imported from LQC), it was shown that the geometry of spacetime near the classical singularity is regular.…”

Section: Introductionmentioning

confidence: 99%

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Semiclassical dynamics of horizons in spherically symmetric collapse

Tavakoli

Marto

Dapor

2014

Int. J. Mod. Phys. D

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In this work, we consider a semiclassical description of the spherically symmetric gravitational collapse with a massless scalar field. In particular, we employ an effective scenario provided by holonomy corrections from loop quantum gravity, to the homogeneous interior spacetime. The singularity that would arise at the final stage of the corresponding classical collapse, is resolved in this context and is replaced by a bounce. Our main purpose is to investigate the evolution of trapped surfaces during this semiclassical collapse. Within this setting, we obtain a threshold radius for the collapsing shells in order to have horizons formation. In addition, we study the final state of the collapse by employing a suitable matching at the boundary shell from which quantum gravity effects are carried to the exterior geometry.

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Section: Conclusion and Discussionmentioning

confidence: 99%

“…Furthermore, some novel features such as evaporation of horizons in the presence of quantum gravity effects were studied in Refs. [14,21]. In addition, it was shown in the Ref.…”

Section: Introductionmentioning

confidence: 97%

Section: Semiclassical Outcomes Of the Collapsementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Semiclassical dynamics of horizons in spherically symmetric collapse

Tavakoli

Marto

Dapor

2014

Int. J. Mod. Phys. D

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“…A straightforward but lengthy calculation reveals that (48) results in f (r v , u) = f (r v ) on the boundary [84]. Furthermore from (47) and the first part of (42) we geṫ…”

Section: Numerical Analysismentioning

confidence: 99%

Collapse and dispersal of a homogeneous spin fluid in Einstein–Cartan theory

2015

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In the present work, we revisit the process of gravitational collapse of a spherically symmetric homogeneous dust fluid which is described by the OppenheimerSnyder (OS) model (Oppenheimer and Snyder in Phys Rev D 56:455, 1939). We show that such a scenario would not end in a spacetime singularity when the spin degrees of freedom of fermionic particles within the collapsing cloud are taken into account. To this purpose, we take the matter content of the stellar object as a homogeneous Weyssenhoff fluid. Employing the homogeneous and isotropic FLRW metric for the interior spacetime setup, it is shown that the spin of matter, in the context of a negative pressure, acts against the pull of gravity and decelerates the dynamical evolution of the collapse in its later stages. Our results show a picture of gravitational collapse in which the collapse process halts at a finite radius, whose value depends on the initial configuration. We thus show that the spacetime singularity that occurs in the OS model is replaced by a non-singular bounce beyond which the collapsing cloud re-expands to infinity. Depending on the model parameters, one can find a minimum value for the boundary of the collapsing cloud or correspondingly a threshold value for the mass content below which the horizon formation can be avoided. Our results are supported by a thorough numerical analysis.

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Gravitational collapse with tachyon field and barotropic fluid

et al. 2013

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A particular class of space-time, with a tachyon field, φ, and a barotropic fluid constituting the matter content, is considered herein as a model for gravitational collapse. For simplicity, the tachyon potential is assumed to be of inverse square form i.e., V (φ) ∼ φ −2 . Our purpose, by making use of the specific kinematical features of the tachyon, which are rather different from a standard scalar field, is to establish the several types of asymptotic behavior that our matter content induces. Employing a dynamical system analysis, complemented by a thorough numerical study, we find classical solutions corresponding to a naked singularity or a black hole formation. In particular, there is a subset where the fluid and tachyon participate in an interesting tracking behaviour, depending sensitively on the initial conditions for the energy densities of the tachyon field and barotropic fluid. Two other classes of solutions are present, corresponding respectively, to either a tachyon or a barotropic fluid regime. Which of these emerges as dominant, will depend on the choice of the barotropic parameter, γ. Furthermore, these collapsing scenarios both have as final state the formation of a black hole.

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Gravitational collapse of quantum matter

Cited by 22 publications

References 23 publications

Semiclassical dynamics of horizons in spherically symmetric collapse

Semiclassical dynamics of horizons in spherically symmetric collapse

Collapse and dispersal of a homogeneous spin fluid in Einstein–Cartan theory

Gravitational collapse with tachyon field and barotropic fluid

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