On horizon structure of bimetric spacetimes

Deffayet, Cédric; Jacobson, Ted

doi:10.1088/0264-9381/29/6/065009

Cited by 63 publications

(94 citation statements)

References 64 publications

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“…In [217,218], de Rham, Gabadadze and Tolley (dRGT) found a loophole and constructed a theory that is free of this pathological sixth mode (this was shown conclusively in [634]). Much work has gone into studying this massive gravity theory: for example studies of cosmological solutions [635][636][637][638][639][640][641][642][643][644][645][646] and black holes [638,[647][648][649][650][651][652] have been undertaken. The theory can also be cast in a vielbein language, as opposed to as a theory of a metric [216,[653][654][655][656][657].…”

Section: A Brief History Of Massive Gravitymentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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After a decade and a half of research motivated by the accelerating universe, theory and experiment have a reached a certain level of maturity. The development of theoretical models beyond Λ or smooth dark energy, often called modified gravity, has led to broader insights into a path forward, and a host of observational and experimental tests have been developed. In this review we present the current state of the field and describe a framework for anticipating developments in the next decade. We identify the guiding principles for rigorous and consistent modifications of the standard model, and discuss the prospects for empirical tests.We begin by reviewing recent attempts to consistently modify Einstein gravity in the infrared, focusing on the notion that additional degrees of freedom introduced by the modification must "screen" themselves from local tests of gravity. We categorize screening mechanisms into three broad classes: mechanisms which become active in regions of high Newtonian potential, those in which first derivatives of the field become important, and those for which second derivatives of the field are important. Examples of the first class, such as f (R) gravity, employ the familiar chameleon or symmetron mechanisms, whereas examples of the last class are galileon and massive gravity theories, employing the Vainshtein mechanism. In each case, we describe the theories as effective theories and discuss prospects for completion in a more fundamental theory. We describe experimental tests of each class of theories, summarizing laboratory and solar system tests and describing in some detail astrophysical and cosmological tests. Finally, we discuss prospects for future tests which will be sensitive to different signatures of new physics in the gravitational sector.The review is structured so that those parts that are more relevant to theorists vs. observers/experimentalists are clearly indicated, in the hope that this will serve as a useful reference for both audiences, as well as helping those interested in bridging the gap between them.

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Section: A Brief History Of Massive Gravitymentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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“…Parameterizing deviations from general relativity: Most of the classical solutions of the bimetric action S gf do not coincide with classical solutions in general relativity [26][27][28][29][30][31][32], except for the class of proportional backgroundsf = c 2ḡ considered here, with c determined by the parameters of the theory. Generic matter couplings of the g and f metrics will drive the solutions away from proportional backgrounds.…”

Section: Some Features Of the G − M Actionmentioning

confidence: 99%

“…Generic cosmological and localized solutions in this theory could show large deviations from solutions in general relativity (GR) although there also exist classes of solutions that are close to GR spacetimes [26][27][28][29][30][31][32]. Below, we will first describe the issues that arise out of interpreting (1.1) as a theory of a spin-2 field coupled to gravity, and summarize our results.…”

Section: Introduction Motivation and Summarymentioning

confidence: 99%

On consistent theories of massive spin-2 fields coupled to gravity

Hassan

Schmidt-May

Strauss

2013

J. High Energ. Phys.

125

177

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We consider the issues that arise out of interpreting the ghost-free bimetric theory as a theory of a spin-2 field coupled to gravity. This requires identifying a gravitational metric and parameterizing deviations of the resulting theory from general relativity. To this end, we first consider the most general bimetric backgrounds for which a massless and a massive spin-2 fluctuation exist, and we compute the most general expression for the Fierz-Pauli mass. These backgrounds coincide with solutions in general relativity. Based on this, we obtain nonlinear extensions of the massive and massless spin-2 fields. The background value of the nonlinear massive field parameterizes generic deviations of the bimetric theory from GR. It is also shown that the most natural nonlinear massless field does not have standard ghost-free matter couplings, and hence cannot represent the gravitational metric. However, an appropriate gravitational metric can still be identified in the weak gravity limit. Hence in the presence of other neutral spin-2 fields, the weak gravity limit is crucial for compatibility with general relativity. We also write down the action in terms of the nonlinear massive spin-2 field and obtain its ghost-free couplings to matter. The discussion is then generalized to multimetric theories.

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“…As we discuss in the next section, π µ may or may not be strongly coupled: it could be strongly coupled within certain radial region, leading to a Vainshtein effect. This branch is the one that concerns us here, so from now on we will only consider static diagonal spherically symmetric solutions in the unitary gauge (see [16] for a similar discussion on bimetric solutions in the unitary gauge).…”

Section: Introductionmentioning

confidence: 99%

Characterizing Vainshtein solutions in massive gravity

Sbisà

Niz

Koyama³

et al. 2012

Phys. Rev. D

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We study static, spherically symmetric solutions in a recently proposed ghost-free model of non-linear massive gravity. We focus on a branch of solutions where the helicity-0 mode can be strongly coupled within certain radial regions, giving rise to the Vainshtein effect. We truncate the analysis to scales below the gravitational Compton wavelength, and consider the weak field limit for the gravitational potentials, while keeping all non-linearities of the helicity-0 mode. We determine analytically the number and properties of local solutions which exist asymptotically on large scales, and of local (inner) solutions which exist on small scales. We find two kinds of asymptotic solutions, one of which is asymptotically flat, while the other one is not, and also two types of inner solutions, one of which displays the Vainshtein mechanism, while the other exhibits a self-shielding behaviour of the gravitational field. We analyse in detail in which cases the solutions match in an intermediate region. The asymptotically flat solutions connect only to inner configurations displaying the Vainshtein mechanism, while the non asymptotically flat solutions can connect with both kinds of inner solutions. We show furthermore that there are some regions in the parameter space where global solutions do not exist, and characterise precisely in which regions of the phase space the Vainshtein mechanism takes place.

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On horizon structure of bimetric spacetimes

Cited by 63 publications

References 64 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

On consistent theories of massive spin-2 fields coupled to gravity

Characterizing Vainshtein solutions in massive gravity

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