Tension perturbations of black brane spacetimes

Traschen, Jennie; Fox, Daniel J. F.

doi:10.1088/0264-9381/21/1/021

Cited by 77 publications

(150 citation statements)

References 19 publications

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“…Strictly speaking, to have γ = 1 (as in general relativity), Ω should be exactly equal to − 1/2. This value is well known for black strings and black branes [9][10][11][12][13][14]. For KK models with Ricci-flat internal spaces, this result does not depend on the size of the extra dimensions [15].…”

Section: Introductionsupporting

confidence: 56%

Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints

et al. 2017

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In a multidimensional Kaluza-Klein model with Ricci-flat internal space, we study the gravitational field in the weak-field limit. This field is created by two coupled sources. First, this is a point-like massive body which has a dust-like equation of state in the external space and an arbitrary parameter Ω of equation of state in the internal space. The second source is a static spherically symmetric massive scalar field centered at the origin where the point-like massive body is. The found perturbed metric coefficients are used to calculate the parameterized post-Newtonian (PPN) parameter γ . We define under which conditions γ can be very close to unity in accordance with the relativistic gravitational tests in the solar system. This can take place for both massive or massless scalar fields. For example, to have γ ≈ 1 in the solar system, the mass of scalar field should be μ 5.05×10 −49 g ∼ 2.83×10 −16 eV. In all cases, we arrive at the same conclusion that to be in agreement with the relativistic gravitational tests, the gravitating mass should have tension: Ω = − 1/2.

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Section: Introductionsupporting

confidence: 56%

Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints

et al. 2017

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“…We can add some intuition to the definition of µ by recalling a previous result [2]. Let g b everywhere, and let g ab be perturbatively close to g o ab .…”

Section: Positivity Theorem For the Gravitational Component Of Tensionmentioning

confidence: 99%

A positivity theorem for gravitational tension in brane spacetimes

Traschen¹

2004

Class. Quantum Grav.

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We study transverse asymptotically flat spacetimes without horizons that arise from brane matter sources. We assume that asymptotically there is a spatial translation Killing vector that is tangent to the brane. Such spacetimes are characterized by a tension, analogous to the ADM mass, which is a gravitational charge associated with the asymptotic spatial translation Killing vector. Using spinor techniques, we prove that the purely gravitational contribution to the spacetime tension is positive definite.

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“…It is worth noting that black strings/branes generalize the known Schwarzschild solution to the multidimensional case (see, e.g., [28][29][30][31] and the corresponding literature therein). Obviously, any multidimensional theory should have such solutions, as they must correspond to the observed astrophysical objects.…”

Section: Introductionmentioning

confidence: 99%

Many-body problem in Kaluza–Klein models with toroidal compactification

2014

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In this paper, we consider a system of gravitating bodies in Kaluza-Klein models with toroidal compactification of the extra dimensions. To simulate the astrophysical objects (e.g., our Sun and pulsars) with energy density much greater than the pressure, we assume that these bodies are pressureless in the external space, i.e., the space we inhabit. At the same time, they may have nonzero parameters ω (ᾱ−3) (ᾱ = 4, . . . , D) in the equations of state in the extra dimensions. We construct the Lagrange function of this many-body system for any value of = ᾱ ω (ᾱ−3) . Moreover, the gravitational tests (PPN parameters, perihelion and periastron advances) require a negligible deviation from the latent soliton value = −(D −3)/2. However, the presence of pressure/tension in the internal space results necessarily in the smearing of the gravitating masses over the internal space and in the absence of KK modes. This looks very unnatural from the point of view of quantum physics.

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Tension perturbations of black brane spacetimes

Cited by 77 publications

References 19 publications

Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints

Weak-field limit of Kaluza–Klein models with spherically symmetric static scalar field: observational constraints

A positivity theorem for gravitational tension in brane spacetimes

Many-body problem in Kaluza–Klein models with toroidal compactification

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