Exact and asymptotic black branes with spherical compactification

Chopovsky, Alexey; Eingorn, Maxim; Zhuk, Alexander

doi:10.1103/physrevd.86.024025

Cited by 8 publications

(32 citation statements)

References 13 publications

(44 reference statements)

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“…To perform it, we should substitute the perturbed metrics (11) and perturbed energy-momentum tensor (9) in the Einstein equation…”

Section: Background and Perturbed Modelsmentioning

confidence: 99%

“…Obviously, such multidimensional theories should not contradict the experimental data, in particular, the well-known gravitational tests in the Solar system: deflection of light, time delay of radar echoes and perihelion precession of Mercury. We investigated this problem in a number of our previous papers [5][6][7][8][9][10][11][12] and one of the main conclusions of these papers is that in the case of Ricci-flat internal spaces, the model with pressureless gravitating mass contradicts gravitational tests [5]. The negative result follows as a consequence of massless fluctuations of the internal space that generate the fifth force [13].…”

Section: Introductionmentioning

confidence: 99%

“…For this type of models, it is possible to achieve agreement with gravitational tests in two cases. First, similar to models with toroidal compactification, we can exclude fluctuations of the internal space with the help of tension (a la blackstrings/blackbranes) [9]. Second, in the absence of tension, we may attain sufficiently short ranges of interaction for the fifth force for large enough mass of radions [8].…”

Section: Introductionmentioning

confidence: 99%

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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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“…To perform it, we should substitute the perturbed metrics (11) and perturbed energy-momentum tensor (9) in the Einstein equation…”

Section: Background and Perturbed Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…tension) in the internal space. The exact form for the metric coefficients was found, e.g., in [2,12] (flat internal space) and in [5] (two-sphere internal space). In the present paper we obtain the metric coefficients in the weak-field limit in the case of the Einstein internal space (flat or curved).…”

Section: Introductionmentioning

confidence: 97%

“…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%

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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Significance of tension for gravitating masses in Kaluza–Klein models

Eingorn¹,

Zhuk²

2012

Physics Letters B

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In this letter, we consider the six-dimensional Kaluza-Klein models with spherical compactification of the internal space. Here, we investigate the case of bare gravitating compact objects with the dustlike equation of statep 0 = 0 in the external (our) space and an arbitrary equation of statep 1 = Ωε in the internal space, whereε is the energy density of the source. This gravitating mass is spherically symmetric in the external space and uniformly smeared over the internal space. In the weak field approximation, the conformal variations of the internal space volume generate the admixture of the Yukawa potential to the usual Newton's gravitational potential. For sufficiently large Yukawa masses, such admixture is negligible and the metric coefficients of the external spacetime coincide with the corresponding expressions of General Relativity. Then, these models satisfy the classical gravitational tests. However, we show that gravitating masses acquire effective relativistic pressure in the external space. Such pressure contradicts the observations of compact astrophysical objects (e.g., the Sun). The equality Ω = −1/2 (i.e. tension) is the only possibility to preserve the dustlike equation of state in the external space. Therefore, in spite of agreement with the gravitational experiments for an arbitrary value of Ω, tension (Ω = −1/2) plays a crucial role for the considered models.

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Exact and asymptotic black branes with spherical compactification

Cited by 8 publications

References 13 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

Significance of tension for gravitating masses in Kaluza–Klein models

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