Dynamics and cosmological constraints on Brans-Dicke cosmology

Hrycyna, Orest; Szydłowski, Marek; Kamionka, Michał

doi:10.1103/physrevd.90.124040

Cited by 36 publications

(52 citation statements)

References 68 publications

(87 reference statements)

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“…is the exact solution for the center manifold, which has the expansion up to fifth order given before (and they satisfy the equations and the initial conditions in (84)). The equation on the center manifold is u = 0.…”

Section: Center Manifold Of B1mentioning

confidence: 99%

Cosmological evolution of two-scalar fields cosmology in the Jordan frame

et al. 2020

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In the present article we study the cosmological evolution of a two-scalar field gravitational theory defined in the Jordan frame. Specifically, we assume one of the scalar fields to be minimally coupled to gravity, while the second field which is the Brans-Dicke scalar field is nonminimally coupled to gravity and also coupled to the other scalar field. In the Einstein frame this theory reduces to a two-scalar field theory where the two fields can interact only in the potential term, which means that the quintom theory is recovered. The cosmological evolution is studied by analyzing the equilibrium points of the field equations in the Jordan frame. We find that the theory can describe the cosmological evolution in large scales, while inflationary solutions are also provided.

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Section: Center Manifold Of B1mentioning

confidence: 99%

Cosmological evolution of two-scalar fields cosmology in the Jordan frame

et al. 2020

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“…This theory provides consistency between the weak field and the strong field regimes [34]. Recent literature indicates the dynamics of SBD gravity in many cosmic problems [35][36][37][38][39][40]. In recent papers [41][42][43], we have explored spherically as well as cylindrically symmetric selfgravitating fluids in SBD gravity and found some interesting results.…”

Section: Introductionmentioning

confidence: 97%

Stellar filaments in self-interacting Brans–Dicke gravity

Sharif

Manzoor

2016

Eur. Phys. J. C

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This paper is devoted to the study of the cylindrically symmetric stellar filaments in self-interacting BransDicke gravity. For this purpose, we construct polytropic filamentary models through a generalized Lane-Emden equation in the Newtonian regime. The resulting models depend upon the values of the cosmological constant (due to the scalar field) along with the polytropic index and represent a generalization of the corresponding models in general relativity. We also investigate the fragmentation of the filaments by exploring the radial oscillations through a stability analysis. This stability criterion depends only upon the adiabatic index.

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“…For zero eigenvalues the system become degenerated and so we can not tell about stability and/or instability of the dynamical system under consideration (see table 1). In context of cosmological models the dynamical system approach is used to obtain ΛCDM phase by more authors [7][8][9][10][11][12][13][14][15][16][17]: Zhou et al are used f (G) gravity to study flat FRW cosmology in [7] where G = R 2 − 4R µν R µν + R µνλη R µνλη is Gauss-Bonnet topological invariant. They are obtained two kinds of stable accelerated solutions called as de Sitter and phantom-like of dark energy regime.…”

Section: Introductionmentioning

confidence: 99%

Dynamical system approach to scalar–vector–tensor cosmology

Ghaffarnejad

Yaraie

2017

Gen Relativ Gravit

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Using scalar-vector-tensor Brans Dicke (VBD) gravity [3] in presence of self interaction BD potential V (φ) and perfect fluid matter field action we solve corresponding field equations via dynamical system approach for flat Friedmann Robertson Walker metric (FRW). We obtained 3 type critical points for ΛCDM vacuum de Sitter era where stability of our solutions are depended to choose particular values of BD parameter ω. One of these fixed points is supported by a constant potential which is stable for ω < 0 and behaves as saddle (quasi stable) for ω ≥ 0. Two other ones are supported by a linear potential V (φ) ∼ φ which one of them is stable for ω = 0.27647. For a fixed value of ω there is at least 2 out of 3 critical points reaching to a unique critical point. Namely for ω = −0.16856(−0.56038) the second (third) critical point become unique with the first critical point. In dust and radiation eras we obtained 1 critical point which never become unique fixed point. In the latter case coordinates of fixed points are also depended to ω. To determine stability of our solutions we calculate eigenvalues of Jacobi matrix of 4D phase space dynamical field equations for de Sitter, dust and radiation eras. We should be point also potentials which support dust and radiation eras must be similar to V (φ) ∼ φ − 1 2 and V (φ) ∼ φ −1 respectively. In short our study predicts that radiation and dust eras of our VBD-FRW cosmology transmit to stable de Sitter state via non-constant potential (effective variable cosmological parameter) by choosing ω = 0.27647.

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Dynamics and cosmological constraints on Brans-Dicke cosmology

Cited by 36 publications

References 68 publications

Cosmological evolution of two-scalar fields cosmology in the Jordan frame

Cosmological evolution of two-scalar fields cosmology in the Jordan frame

Stellar filaments in self-interacting Brans–Dicke gravity

Dynamical system approach to scalar–vector–tensor cosmology

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