Significance of tension for gravitating masses in Kaluza–Klein models

Eingorn, Maxim; Zhuk, Alexander

doi:10.1016/j.physletb.2012.08.031

Cited by 7 publications

(10 citation statements)

References 17 publications

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“…However, fluctuations of background matter concentrate around the gravitating mass and the bare gravitating mass gets covered by this coat to attain effective relativistic pressure in the external space. Certainly, this contradicts the observations (e.g., Sun does not have such relativistic pressure) and the only way to avoid such problem is to introduce, again, tension in the internal space [10,14].…”

Section: Introductionmentioning

confidence: 91%

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Weak-Field Limit of a Kaluza-Klein Model with a Nonlinear Perfect Fluid

Yalçınkaya

Zhuk

2019

Gravit. Cosmol.

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The main purpose of our paper is to construct a viable Kaluza-Klein model satisfying the observable constraints. To this end, we investigate the six-dimensional model with spherical compactification of the internal space. Background matter is considered in the form of a perfect fluid with non-linear equations of state both in the external/our and internal spaces and the model is set to include an additional bare cosmological constant Λ 6 . In the weak-field approximation, the background is perturbed by pressureless gravitating mass that is a static point-like particle. The non-linearity of the equations of state of a perfect fluid makes it possible to solve simultaneously a number of problems. The demand that the parameterized post-Newtonian parameter γ be equal to 1 in this configuration, first, ensures compatibility with gravitational tests in the Solar system (deflection of light and time delay of radar echoes) at the same level of accuracy as General Relativity. Second, it translates into the absence of internal space variations so that the gravitational potential coincides exactly with the Newtonian one, securing the absence of the fifth force. Third, the gravitating mass remains pressurless in the external space as in the standard approach to non-relativistic astrophysical objects and meanwhile, acquires effective tension in the internal space. *

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Section: Introductionmentioning

confidence: 91%

“…To get it we should put B 1 /A 1 = 1 [15]; this is our fine tuning condition. As it follows from (13) and (14), this takes place if δε + δp 0 + 2δp 1 +ρc 2 = 0 ,…”

Section: Background and Perturbed Modelsmentioning

confidence: 99%

Weak-Field Limit of a Kaluza-Klein Model with a Nonlinear Perfect Fluid

Yalçınkaya

Zhuk

2019

Gravit. Cosmol.

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“…Additionally, taking into account that h µν = 0 for µ ν and h µn = 0, we arrive at the conclusion that the perturbed metric retains the block-diagonal form. In our previous papers the block-diagonal form of the perturbed metric was accepted either as an ansatz [7] or as a consequence of the assumption of uniform smearing (over the internal space) of the gravitating mass [3,5,6]. In the present article, we demonstrate for the considered model that this statement follows directly from the Einstein equation and gauge condition without both of these assumptions.…”

Section: Weak-field Limit Of Black Strings and Black Branesmentioning

confidence: 55%

“…It is well known that compact nonrelativistic astrophysical objects such as our Sun have the dust-like EoS since the pressure inside them is much less than the energy density. In our paper [6] we have shown that in the case of multidimensional models the gravitating masses acquire effective relativistic pressure in the external space. Certainly, such pressure contradicts the observations.…”

Section: Weak-field Limit Of Black Strings and Black Branesmentioning

confidence: 81%

“…We intend to check whether KK models adequately describe astrophysical objects such as our Sun and, additionally, to show that they can correspond to the conventional cosmological model. In a number of our previous papers (see, e.g., [2,3,4,5,6,7]) we have already discussed the astrophysical aspects of KK models. However, in these papers we have imposed additional conditions on considered models, e.g., the preservation of the blockdiagonal form of the perturbed metric as well as the assumption Email addresses: akarsuo@itu.edu.tr (Özgür Akarsu), a.chopovsky@yandex.ru (Alexey Chopovsky), ai.zhuk2@gmail.com (Alexander Zhuk) on the uniform smearing of the gravitating body over the internal space.…”

Section: Introductionmentioning

confidence: 99%

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Black branes and black strings in the astrophysical and cosmological context

2018

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We consider Kaluza-Klein models where internal spaces are compact flat or curved Einstein spaces. This background is perturbed by a compact gravitating body with the dust-like equation of state (EoS) in the external/our space and an arbitrary EoS parameter Ω in the internal space. Without imposing any restrictions on the form of the perturbed metric and the distribution of the perturbed energy densities, we perform the general analysis of the Einstein and conservation equations in the weak-field limit. All conclusions follow from this analysis. For example, we demonstrate that the perturbed model is static and perturbed metric preserves the blockdiagonal form. In a particular case Ω = −1/2, the found solution corresponds to the weak-field limit of the black strings/branes. The black strings/branes are compact gravitating objects which have the topology (four-dimensional Schwarzschild spacetime)× (d-dimensional internal space) with d ≥ 1. We present the arguments in favour of these objects. First, they satisfy the gravitational tests for the parameterized post-Newtonian parameter γ at the same level of accuracy as General Relativity. Second, they are preferable from the thermodynamical point of view. Third, averaging over the Universe, they do not destroy the stabilization of the internal space. These are the astrophysical and cosmological aspects of the black strings/branes.

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Kaluza–Klein models with spherical compactification: observational constraints and possible examples

Eingorn

Fakhr

Zhuk

2013

Class. Quantum Grav.

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We consider Kaluza–Klein models with background matter in the form of a multicomponent perfect fluid. This matter provides spherical compactification of the internal space with an arbitrary number of dimensions. The gravitating source has the dust-like equation of state in the external/our space and an arbitrary equation of state (with the parameter Ω) in the internal space. In the single-component case, tension (Ω = −1/2) is the necessary condition to satisfy both the gravitational tests in the solar system and the thermodynamical observations. In the multicomponent case, we propose two models satisfying both of these observations. One of them also requires tension Ω = −1/2, but the second one is of special interest because it is free of tension, i.e. Ω = 0. To obtain this result, we need to impose certain conditions.

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Significance of tension for gravitating masses in Kaluza–Klein models

Cited by 7 publications

References 17 publications

Weak-Field Limit of a Kaluza-Klein Model with a Nonlinear Perfect Fluid

Weak-Field Limit of a Kaluza-Klein Model with a Nonlinear Perfect Fluid

Black branes and black strings in the astrophysical and cosmological context

Kaluza–Klein models with spherical compactification: observational constraints and possible examples

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