Nonperturbative strong-field effects in tensor-scalar theories of gravitation

Damour, Thibault; Esposito-Farèse, Gilles

doi:10.1103/physrevlett.70.2220

Cited by 873 publications

(1,551 citation statements)

References 15 publications

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“…Due to the peculiar "effacement" properties of strong-field effects taking place in General Relativity [24], the fact that pulsar data probe the strong-gravitational-field regime can only be seen when contrasting Einstein's theory with more general theories. In particular, it has been found in tensor-scalar theories [26] that a self-gravity as strong as that of a neutron star can naturally (i.e. without fine tuning of parameters) induce order-unity deviations from general relativistic predictions in the orbital dynamics of a binary pulsar thanks to the existence of nonperturbative strong-field effects.…”

Section: Tests Of the Dynamics Of The Gravitational Field In The Stromentioning

confidence: 99%

“…For instance, as we said above, a test involvingṖ b probes the propagation (and helicity) properties of the gravitational interaction. But a test involving, say, k, γ, r or s probes (as shown by combining the results of [13] and [26]) strong self-gravity effects independently of radiative effects.…”

Section: Tests Of the Dynamics Of The Gravitational Field In The Stromentioning

confidence: 99%

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Gravitation and Experiment

Damour¹

2007

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The confrontation between Einstein's gravitation theory and experimental results, notably binary pulsar data, is summarized and its significance discussed. Experiment and theory agree at the 10 −3 level. All the basic structures of Einstein's theory (coupling of gravity to matter; propagation and self-interaction of the gravitational field, including in strong-field conditions) have been verified. However, some recent theoretical findings (cosmological relaxation toward zero scalar couplings) suggest that the present agreement between Einstein's theory and experiment might be naturally compatible with the existence of a long-range scalar contribution to gravity (such as the dilaton, or a moduli field of string theory). This provides a new theoretical paradigm, and new motivations for improving the experimental tests

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Section: Tests Of the Dynamics Of The Gravitational Field In The Stromentioning

confidence: 99%

Section: Tests Of the Dynamics Of The Gravitational Field In The Stromentioning

confidence: 99%

Gravitation and Experiment

Damour¹

2007

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“…it is characterized by a unique free parameter α 2 0 = (2ω BD + 3) −1 and all its predictions differ from those of general relativity by quantities of order α 2 0 [10]. Solar system experiments set strict limits in the value of the BransDicke parameter ω BD i.e.…”

Section: Introductionmentioning

confidence: 99%

Probing strong-field scalar-tensor gravity with gravitational wave asteroseismology

2004

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We present an alternative way of tracing the existence of a scalar field based on the analysis of the gravitational wave spectrum of a vibrating neutron star. Scalar-tensor theories in strong-field gravity can potentially introduce much greater differences in the parameters of a neutron star than the uncertainties introduced by the various equations of state. The detection of gravitational waves from neutron stars can set constraints on the existence and the strength of scalar fields. We show that the oscillation spectrum is dramatically affected by the presence of a scalar field, and can provide unique confirmation of its existence.

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“…(3.37) 39) where N ≡ N (Q) = ln[a(Q(t))] and we have made the substitution This general solution contains three free parameters (N , α and c 1 ). To keep the solution as general as possible it is useful to just fix one free parameter in terms of the other two.…”

Section: Uncoupled Quintessencementioning

confidence: 99%

“…19 the best fit plot with α Q = 0. The post-Newtonian parameterγ is related to α Q 0 (≡ χ) through the relation [39] …”

Section: Confronting Models With Datamentioning

confidence: 99%

Inflation and quintessence: theoretical approach of cosmological reconstruction

Neupane

Scherer

2008

J. Cosmol. Astropart. Phys.

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In the first part of this paper, we outline the construction of an inflationary cosmology in the framework where inflation is described by a universally evolving scalar field φ with potential V (φ). By considering a generic situation that inflaton attains a nearly constant velocity, during inflation, m −1 P |dφ/dN | ≡ α + β exp(βN ) (where N ≡ ln a is the e-folding time), we reconstruct a scalar potential and find the conditions that have to satisfied by the (reconstructed) potential to be consistent with the WMAP inflationary data. The consistency of our model with WMAP result (such as n s = 0.951 +0.015 −0.019 and r < 0.3) would require 0.16 < α < 0.26 and β < 0. The running of spectral index, α ≡ dn s /d ln k, is found to be small for a wide range of α.In the second part of this paper, we introduce a novel approach of constructing dark energy within the context of the standard scalar-tensor theory. The assumption that a scalar field might roll with a nearly constant velocity, during inflation, can also be applied to quintessence or dark energy models. For the minimally coupled quintessence, α Q ≡ dA(Q)/d(κQ) = 0 (where A(Q) is the standard matter-quintessence coupling), the dark energy equation of state in the range −1 ≤ w DE < −0.82 can be obtained for 0 ≤ α < 0.63. For α < 0.1, the model allows for only modest evolution of dark energy density with redshift. We also show, under certain conditions, that the α Q > 0 solution decreases the dark energy equation of state w Q with decreasing redshift as compared to the α Q = 0 solution. This effect can be opposite in the α Q < 0 case. The effect of the matterquintessence coupling can be significant only if |α Q | 0.1, while a small coupling |α Q | < 0.1 will have almost no effect on cosmological parameters, including Ω Q , w Q and H(z). The best fit value of α Q in our model is found to be α Q ≃ 0.06, but it may contain significant numerical errors, viz α Q = 0.06 ± 0.35, which thereby implies the consistency of our model with general relativity (for which α Q = 0) at 1σ level.

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Nonperturbative strong-field effects in tensor-scalar theories of gravitation

Cited by 873 publications

References 15 publications

Gravitation and Experiment

Gravitation and Experiment

Probing strong-field scalar-tensor gravity with gravitational wave asteroseismology

Inflation and quintessence: theoretical approach of cosmological reconstruction

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