Vacuum-field solutions in the brans-dicke theory

O'Hanlon, John; Tupper, B. O. J.

doi:10.1007/bf02743602

Cited by 121 publications

(100 citation statements)

References 2 publications

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“…Further on, we assume that α > 0 for stability of the theory. The two scaling solutions in the vanishing potential case (the pure Brans-Dicke theory) are [63] |Φ| ∝ |t| r , r = 1 ± 3 1 + 1 6α…”

Section: αmentioning

confidence: 99%

Scalar–tensor models of normal and phantom dark energy

Gannouji

Polarski

André

et al. 2006

J. Cosmol. Astropart. Phys.

223

193

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We consider the viability of dark energy (DE) models in the framework of the scalar-tensor theory of gravity, including the possibility to have a phantom DE at small redshifts z as admitted by supernova luminosity-distance data. For small z, the generic solution for these models is constructed in the form of a power series in z without any approximation. Necessary constraints for DE to be phantom today and to cross the phantom divide line p = −ρ at small z are presented. Considering the Solar System constraints, we find for the postNewtonian parameters that γ P N < 1 and γ P N,0 ≈ 1 for the model to be viable, and β P N,0 > 1 (but very close to 1) if the model has a significantly phantom DE today. However, prospects to establish the phantom behaviour of DE are much better with cosmological data than with Solar System experiments. Earlier obtained results for a Λ-dominated universe with the vanishing scalar field potential are extended to a more general DE equation of state confirming that the cosmological evolution of these models rule them out. Models of currently fantom DE which are viable for small z can be easily constructed with a constant potential; however, they generically become singular at some higher z. With a growing potential, viable models exist up to an arbitrary high redshift.

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Section: αmentioning

confidence: 99%

Scalar–tensor models of normal and phantom dark energy

Gannouji

Polarski

André

et al. 2006

J. Cosmol. Astropart. Phys.

223

193

View full text Add to dashboard Cite

show abstract

“…Such behaviour would necessarily entail a variation of φ in space as well as time. Solutions have been found for specific ω in which φ is inhomogeneous 84) , so such models are clearly possible in principle. We must also allow for the possibility that φ may vary interior to R m but on a slower or faster timescale than the background.…”

Section: Variations Of Gravitational Memorymentioning

confidence: 99%

Primordial Black Holes and Gravitational Memory

Carr

Goymer

1999

Prog. Theor. Phys. Suppl.

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We discuss the various ways in which primordial black holes may have formed in the early Universe and how the effects of such black holes can be used to place constraints on cosmological models. We show that such constraints may be severely modified if the value of the gravitational "constant" G varies with cosmological epoch, a possibility which arises in many scenarios for the early Universe. The nature of the modification depends upon whether the value of G near a black hole maintains the value it had at its formation epoch (corresponding to gravitational memory) or whether it tracks the background cosmological value. This is still uncertain but we discuss various approaches which might help to resolve the issue.

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“…This vacuum BD solution (where d 2 = 3 is determined from the generalized Friedmann equation) was first obtained by O'Hanlon and Tupper (1972). We note that for large values of ω 0 ,…”

Section: Brans-dicke Theorymentioning

confidence: 65%

Qualitative Properties of Scalar-Tensor Theories of Gravity

Coley¹

1999

General Relativity and Gravitation

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The qualitative properties of spatially homogeneous stiff perfect fluid and minimally coupled massless scalar field models within general relativity are discussed. Consequently, by exploiting the formal equivalence under conformal transformations and field redefinitions of certain classes of theories of gravity, the asymptotic properties of spatially homogeneous models in a class of scalar-tensor theories of gravity that includes the Brans-Dicke theory can be determined. For example, exact solutions are presented, which are analogues of the general relativistic Jacobs stiff perfect fluid solutions and vacuum plane wave solutions, which act as past and future attractors in the class of spatially homogeneous models in Brans-Dicke theory.

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Vacuum-field solutions in the brans-dicke theory

Cited by 121 publications

References 2 publications

Scalar–tensor models of normal and phantom dark energy

Scalar–tensor models of normal and phantom dark energy

Primordial Black Holes and Gravitational Memory

Qualitative Properties of Scalar-Tensor Theories of Gravity

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