Gravitational Collapse in the EGB Gravity

Chatterjee, Ayan; Ghosh, Avirup; Jaryal, Suresh C.

doi:10.48550/arxiv.2108.11680

Cited by 1 publication

(3 citation statements)

References 49 publications

(111 reference statements)

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“…To study these changes, let t µ = µ − C n µ is tangent to the MTT. Then, t µ becomes spacelike or null depending on the quantity C, which is given by [30,38]:…”

Section: Horizon Formation From Gravitational Collapsementioning

confidence: 99%

“…The marginally bound collapse model of homogeneous dust in 4d EGB was discussed in [27]. The n ≥ marginally bound collapse model of inhomogeneous dust is discussed in [28,29], whereas, [30] discusses generic models. Naturally homogeneous, isotropic models cannot capture the intricacies of collapse scenarios, here we consider the process of gravitational collapse of a distribution of inhomogeneous dust bounded by a spherical surface which are either marginally bound or are bounded.…”

Section: Introductionmentioning

confidence: 99%

“…Following [32,33,34,35], the horizon shall be defined as a MTT. A crucial feature of MTT, which shall be of great importance in our study is, they do not carry any specific signature, and hence, can be used to infer if the horizon is growing (for which the tangent vector to MTT shall be spacelike), of if it is in equilibrium (when the MTT carries null signature) [30,36,37]. Our task will be to locate the the spherical MTT during the physical collape process, and to track the variations in the parameter space which affect the dynamics of MTT.…”

Section: Introductionmentioning

confidence: 99%

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Spherical Gravitational Collapse in 4D Einstein- Gauss- Bonnet theory

Jaryal¹,

Chatterjee²

2022

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In this paper, we study spherical gravitational collapse of inhomogeneous pressureless matter in n → 4d Einstein-Gauss-Bonnet gravity. The collapse leads to either a black hole or a massive naked singularity depending on time of formation of trapped surfaces. More precisely, horizon formation and its time development is controlled by relative strengths of the Gauss-Bonnet coupling (λ) and the mass function F (r, t) of collapsing sphere. We find that, if there is no black hole on the initial Cauchy hypersurface and F (r, t) < 2 √ λ, the central singularity is massive and naked. When this inequality is equalised or reversed, the central singularity is always censored by spacelike/timelike spherical marginally trapped surface of topology S 2 × R, which eventually becomes null and coincides with the event horizon at equilibrium. These conclusions are verified for a wide class of mass profiles admitting different initial velocity conditions.

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“…To study these changes, let t µ = µ − C n µ is tangent to the MTT. Then, t µ becomes spacelike or null depending on the quantity C, which is given by [30,38]:…”

Section: Horizon Formation From Gravitational Collapsementioning

confidence: 99%