A theoretical construction of thin shell wormhole from tidal charged black hole

Rahaman, Farook; Kalam, Mehedi; Rahman, K. A.; Chakraborti, S.

doi:10.1007/s10714-007-0427-1

Cited by 34 publications

(38 citation statements)

References 16 publications

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“…Using these values in Eqs. (12) and (25), the dynamical equation and the second derivative of potential for the thin-shell wormhole satisfied by the throat radius becomes…”

Section: Charged Black String Thin-shell Wormholesmentioning

confidence: 99%

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Stability analysis of thin-shell wormholes from charged black string

Sharif

Azam

2013

J. Cosmol. Astropart. Phys.

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In this paper, we construct thin-shell wormholes from charged black string through cut and paste procedure and investigate its stability. We assume modified generalized Chaplygin gas as a dark energy fluid (exotic matter) present in the thin layer of matter-shell. The stability of these constructed thin-shell wormholes is investigated in the scenario of linear perturbations. We conclude that static stable as well as unstable configurations are possible for cylindrical thin-shell wormholes.

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“…Using these values in Eqs. (12) and (25), the dynamical equation and the second derivative of potential for the thin-shell wormhole satisfied by the throat radius becomes…”

Section: Charged Black String Thin-shell Wormholesmentioning

confidence: 99%

“…For this purpose, we take A = 0 and β = 0.2, 0.6, 1 in Eq. (12) and results are shown in Figures 4-6. When β = 0.2, we have only unstable solution for |Q| = 0, 0.7Q c , while for |Q| = 0.999Q c there exist three solutions two are unstable and one is stable.…”

Section: Charged Black String Thin-shell Wormholesmentioning

confidence: 99%

Stability analysis of thin-shell wormholes from charged black string

Sharif

Azam

2013

J. Cosmol. Astropart. Phys.

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“…The dynamical analysis in [13,14,15] was generalized by considering solutions with electrical charge [16], solutions in the presence of a cosmological constant [17], and spherically symmetric dynamical solutions [18]. More recently, by using the cut and paste technique, several solutions were analyzed, such as, the dynamics of non rotating cylindrical thin-shell wormholes [19], charged thin-shell Lorentzian wormholes in dilaton gravity [20], five dimensional thin-shell wormholes in Einstein-Maxwell theory with a Gauss-Bonnet term [21], solutions in higher dimensional Einstein-Maxwell theory [22], thin-shell wormholes associated with global cosmic strings [23], solutions in heterotic string theory [24], spherical thin-shell wormholes supported by a Chaplygin gas [25], a new class of thin-shell wormhole by surgically grafting two black hole solutions localized on a three brane in five dimensional gravity in the Randall-Sundrum scenario [26], and spherically symmetric thin-shell wormholes in a string cloud background in (3+1)-dimensional spacetime were also analyzed [27]. Other wormhole solutions have been analyzed in [28,29,30,31].…”

Section: Introductionmentioning

confidence: 99%

Plane symmetric thin-shell wormholes: Solutions and stability

Lemos¹,

Lobo

2008

Phys. Rev. D

139

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Using the cut-and-paste procedure, we construct static and dynamic plane symmetric wormholes by surgically grafting together two spacetimes of plane symmetric vacuum solutions with a negative cosmological constant. These plane symmetric wormholes can be interpreted as domain walls connecting different universes, having planar topology, and upon compactification of one or two coordinates, cylindrical topology or toroidal topology, respectively. A stability analysis is carried out for the dynamic case by taking into account specific equations of state, and a linearized stability analysis around static solutions is also explored. It is found that thin shell wormholes made of a dark energy fluid or of a cosmological constant fluid are stable, while thin shell wormholes made of phantom energy are unstable.

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“…Thus, β and the dimensionless anisotropy parameter [25,26] ∆ ≡ (p t −p r )/ρ = β−α are both positive (at least in the region adjacent to the throat). Using (14), the first two lines (13) and (15) yield…”

Section: Redshift-free Static Wormholesmentioning

confidence: 99%

“…The aim of this section is to derive closed-form wormhole solutions of type I and II. The barotropic equations (14) no longer are suitable as ansatzes, so we will introduce a new systematic approach.…”

Section: Static Wormholes With Redshift Effectsmentioning

confidence: 99%

Confined-exotic-matter wormholes with no gluing effects—Imaging supermassive wormholes and black holes

Azreg‐Aïnou

2015

J. Cosmol. Astropart. Phys.

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We classify wormholes endowed with redshift effects and finite mass into three types. Type I wormholes have their radial pressure dying out faster, as one moves away from the throat, than any other component of the stress-energy and thus violate the least the local energy conditions. In type II (resp. III) wormholes the radial and transverse pressures are asymptotically proportional and die out faster (resp. slower) than the energy density. We introduce a novel and generalizable method for deriving, with no cutoff in the stress-energy or gluing, a class of each of the three wormhole types. We focus on type I wormholes and construct different asymptotically flat solutions with finite, upperand lower-bounded, mass M . It is observed that the radial pressure is negative, and the null energy condition is violated, only inside a narrow layer, adjacent to the throat, of relative spacial extent ǫ. Reducing the relative size of the layer, without harming the condition of traversability, yields an inverse square law of ǫ versus M for supermassive wormholes. We show that the diameter of the shadow of this type I supermassive wormhole overlaps with that of the black hole candidate at the center of the Milky Way and that the recent derivation, using the up-to-date millimeter-wavelength very long baseline interferometry made in Astrophys. J. 795 134 (2014) [arXiv:1409.4690], remains inconclusive.We show that redshift-free wormholes, with positive energy density, have one of their barotropic equations of state in the phantom regime (at least in the region adjacent to the throat), have their stress energy tensor traceless, and are anisotropic. They are all type III wormholes having their variable equations of state approaching 1 and −1 at spatial infinity. We also introduce a new approach for deriving new redshift-free wormholes.

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A theoretical construction of thin shell wormhole from tidal charged black hole

Cited by 34 publications

References 16 publications

Stability analysis of thin-shell wormholes from charged black string

Stability analysis of thin-shell wormholes from charged black string

Plane symmetric thin-shell wormholes: Solutions and stability

Confined-exotic-matter wormholes with no gluing effects—Imaging supermassive wormholes and black holes

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