Intra-Galactic Thin Shell Wormhole and Its Stability

Bochicchio, Ivana; Laserra, Ettore

doi:10.1007/s10773-013-1677-1

Cited by 5 publications

(2 citation statements)

References 77 publications

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“…The use of variable EoS could boost the stability of thin-shell models of intra-galactic wormholes based on the Mannheim-Kazanas-de Sitter solution [39]. Also, it could improve the stability of truncated Morris-Thorne wormhole models involving dynamical thin-shell boundary [16].…”

Section: Resultsmentioning

confidence: 99%

Note on linearized stability of Schwarzschild thin-shell wormholes with variable equations of state

Varela

2015

Phys. Rev. D

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We discuss how the assumption of variable equation of state (EoS) allows the elimination of the instability at equilibrium throat radius a0 = 3M featured by previous Schwarzschild thin-shell wormhole models. Unobstructed stability regions are found for three choices of variable EoS. Two of these EoS entail linear stability at every equilibrium radius. Particularly, the thin-shell remains stable as a0 approaches the Schwarzschild radius 2M . A perturbative analysis of the wormhole equation of motion is carried out in the case of variable Chaplygin EoS. The squared proper angular frequency ω 2 0 of small throat oscillations is linked with the second derivative of the thin-shell potential. In various situations ω 2 0 remains positive and bounded in the limit a0 → 2M .PACS indexing codes: 04.20.Jb Complementary aspects of thick shells and thin shells appear in the sequential development of analytical gravastar models. Mazur and Mottola [7] argued for the thermodynamic stability of a gravastar model involving a (relatively thin) finite-thickness shell bounded by two thin shells. Visser and Wiltshire [8] considered the dynamical stability of a thin-shell gravastar retaining most of the original features of Mazur and Mottola's model. Chirenti and Rezzola [9] studied the stability of a spherical thick-shell gravastar model submitted to axial perturbations. The analysis of non-radial gravastar perturbations was extended by Pani et al. [10], who combined standard perturbation theory with Israel's formalism to describe polar perturbations of non-rotating, thin-shell gravastar models.The interplay of thick shells and thin shells emerges in other dynamical contexts as well. Garfinkle and Gregory [11] expanded the equations of a thick gravitating wall in powers of the thickness of the wall. They found that the zeroth-order equations reproduce the thin-wall approximation for domain walls provided by the Israel formalism. Also, they used the first-order thick-wall equations to modify thin-wall equations and discuss the motion of domain walls. Khakshournia and Mansouri [12] determined that the zeroth-order approximation of the equations of motion of a spherical dustlike thick shell coincide with equations arising from the thin-shell formalism. They also found that the effect of thickness is to speed up the collapse of the shell. More recently, Drobov and Tegai [13] added anisotropy to a thick wall of fluid and obtained the appropriate thin-shell limit.Garcia et al. (GLV) [14] have summarized the status of the energy conditions of standard general relativity in connection with the theoretical construction of wormholes. These hypothetical tunnels in spacetime are supported by "exotic matter" which violates all the pointwise and all the averaged energy conditions. To minimize the extent of this problem, researchers have considered truncated Morris-Thorne models featuring a cut-off of the stress-energy, and a junction interface. (See, for example, [15,16].) This junction constitutes a thin-shell or a boundary surface depending on ...

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Section: Resultsmentioning

confidence: 99%

Note on linearized stability of Schwarzschild thin-shell wormholes with variable equations of state

Varela

2015

Phys. Rev. D

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“…Exactly the same arguments hold for the full MK solution B(r) = 1 − 2M r + γr − kr 2 as well because there now appears two horizons for k > 0 at radii given by (for details, see Ref. [101]):…”

Section: Critical Reappraisalsmentioning

confidence: 59%

Mass decomposition of SLACS lens galaxies in Weyl conformal gravity

2016

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We study here, using the Mannheim-Kazanas solution of Weyl conformal theory, the mass decomposition in the representative subsample of 57 earlytype elliptical lens galaxies of the Sloan Lens Advanced Camera for Surveys (SLACS) on board the Hubble Space Telescope (HST). We begin by showing that the solution need not be an exclusive solution of conformal gravity but can also be viewed as a solution of a class of f (R) gravity theories coupled to non-linear electrodynamics thereby rendering the ensuing results more universal. Since lensing involves light bending, we shall first show that the solution adds to Schwarzschild light bending caused by the luminous mass (M * ) a positive contribution +γR contrary to the previous results in the literature, thereby resolving a long standing problem. The cause of the error is critically examined. Next, applying the expressions for light bending together with an input equating Einstein and Weyl angles, we develop a novel algorithm for separating the luminous component from the total lens mass (luminous+dark) within the Einstein radius. Our results indicate that the luminous mass estimates differ from the observed total lens masses by a linear proportionality factor across the subsample, which qualitatively agrees with the common conclusion from a number of different simulations in the literature. In quantitative detail, we observe that the ratios of luminous over total lens mass (f * ) within the Einstein radius of individual galaxies take on values near unity, many of which remarkably fall inside or just marginally outside the specified error bars obtained from a simulation based on the Bruzual-Charlot stellar population synthesis model together with the Salpeter Intitial Mass Function (IMF) favored on the ground of metallicity [Grillo et al., Astron. Astrophys. 501, 461(2009) average dark matter density ρ av of individual galaxies within their respective Einstein spheres. To our knowledge, the present approach, being truly analytic, seems to be the first of its kind attempting to provide a new decomposition scheme distinct from the simulational ones.

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Linear stability analysis of a rotating thin-shell wormhole

Tsukamoto

Kokubu

2018

Phys. Rev. D

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We cut and paste two Bañados-Teitelboim-Zanelli (BTZ) spacetimes at a throat by the Darmois-Israel method to construct a rotating wormhole with a thin shell filled with a barotropic fluid. The thin shell at the throat and both sides of the throat corotate. We investigate the linear stability of the thin shell of the rotating wormhole against radial perturbations. We show that the wormhole becomes more and more stable the larger its angular momentum is until the angular momentum reaches a critical value and that the behavior of a condition for stability significantly changes when the angular momentum exceeds the critical value. We find that the overcritical rotating wormhole has the radius of the thin shell, which is stable regardless of the equation of state for the barotropic fluid.

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Intra-Galactic Thin Shell Wormhole and Its Stability

Cited by 5 publications

References 77 publications

Note on linearized stability of Schwarzschild thin-shell wormholes with variable equations of state

Note on linearized stability of Schwarzschild thin-shell wormholes with variable equations of state

Mass decomposition of SLACS lens galaxies in Weyl conformal gravity

Linear stability analysis of a rotating thin-shell wormhole

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