Complete density perturbations in the Jordan-Fierz-Brans-Dicke theory

Cembranos, J. A. R.; Cruz-Dombriz, Álvaro de la; Garcia, L.

doi:10.1103/physrevd.88.123507

Cited by 12 publications

(8 citation statements)

References 156 publications

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“…Then, the investigation of the linear and nonlinear growth of the matter density perturbations may be able to differentiate scalar-tensor theories, even though they could realize the very similar expansion history of the universe, as has been investigated for the various scalar-tensor/modified gravity theories (see e.g., Refs. [45][46][47][48][49][50]). We hope to come back to these issues in our future publications.…”

Section: Discussionmentioning

confidence: 99%

Solutions in the scalar-tensor theory with nonminimal derivative coupling

2014

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We present black hole type solutions in the scalar-tensor theory with nonminimal derivative coupling to the Einstein tensor. The effects of the nonminimal derivative coupling appear in the large scales, while the solutions approach those in the Einstein gravity in the small scales. For the particular coupling constant tuned to the inverse of the cosmological constant, the scalar field becomes trivial and the solutions in the Einstein gravity are recovered. For the other coupling constant, more general solutions can be obtained. If the two-dimensional maximally symmetric space is a two-sphere, the spacetime structure approaches anti-de Sitter spacetime in the large scales. On the other hand, if the two-dimensional space is a two-hyperboloid, the spacetime approaches de Sitter (AdS) spacetime. If it is a flat space, the cosmological constant affects only the amplitude of the scalar field. The extension to the higher-dimensional case is also straightforward. For a certain range of the negative cosmological constant, thermodynamic properties of a black hole are very similar to those of the Schwarzschild-AdS black hole in the Einstein gravity.

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Section: Discussionmentioning

confidence: 99%

Solutions in the scalar-tensor theory with nonminimal derivative coupling

2014

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“…The differential equation (15) gives the evolution of the density contrast δ with z. This equation is solved numerically from z = 1100 to the present epoch z = 0 with standard initial conditions as given by Cembranos et al [49] and Mehrabi et al [50] like δ (z = 1100) = 0.001 and δ ′ (z = 1100) = 0. The value of the constant A, which is actually Ω m0 is taken as 0.286 [43].…”

Section: A Slowly Varying Jerkmentioning

confidence: 99%

“…grow with the evolution (increase with a). Like the interacting case presented in section (4), here also the initial conditions are chosen at z = 1100 as given by Cembranos et al [49] and Mehrabi et al [50], but the plots are given between a = 0.09 (corresponding to z = 10) and a = 1 for the sake of better resolution.…”

Section: A Varying Jerkmentioning

confidence: 99%

Density perturbation in the models reconstructed from jerk parameter

Sinha

Banerjee

2018

Gen Relativ Gravit

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“…The authors in [44] have already studied the evolution of the density contrast for Jordan-Fierz-Brans-Dicke theories in a Friedmann-Lemaitre-Robertson-Walker Universe. Following their work , we are going to investigate the density perturbation of the model based on the phase plane analysis.…”

Section: Introductionmentioning

confidence: 99%

“…In Sect. 3 following [44], we implement the metric perturbation and drive the perturbed equations. In Sect.…”

Section: Introductionmentioning

confidence: 99%

Visualization of cosmological density fluctuations with phase space analysis: case study: Brans–Dicke theory

Salehi

Farajollahi

2019

Eur. Phys. J. C

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Cosmological perturbation theory is a powerful tool to understanding the large-scale structure of the Universe. However, the set of field equations describes the general linear perturbations for the cosmological models is highly nonlinear and coupled where no analytical solution can be found. It is only after some simplification and numerical computation that we obtain limited solutions. On way around is to employ the phase space analysis and investigate the asymptotic stability of the model. The advantage of using this approach is that the system of field equations become simpler to solve numerically. The algorithm also determines the stability of the system. Here, we apply this approach in Brans-Dicke cosmology and study the attractor solutions after fitting the model with the SNeIa observational data. As a result, the model confirms small fluctuations of energy density. The model also predicts current universe acceleration confirmed by observation and benefits from phase space analysis that the new dynamical variables are independent of the model initial conditions.

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Complete density perturbations in the Jordan-Fierz-Brans-Dicke theory

Cited by 12 publications

References 156 publications

Solutions in the scalar-tensor theory with nonminimal derivative coupling

Solutions in the scalar-tensor theory with nonminimal derivative coupling

Density perturbation in the models reconstructed from jerk parameter

Visualization of cosmological density fluctuations with phase space analysis: case study: Brans–Dicke theory

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