On black holes in massive gravity

Berezhiani, Lasha; Chkareuli, Giga; Rham, Claudia de; Gabadadze, Gregory; Tolley, Andrew J.

doi:10.1103/physrevd.85.044024

Cited by 163 publications

(160 citation statements)

References 31 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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“…[17]) enables us to find new solutions in massive gravity. In addition, this choice is useful for avoiding potential ghost instabilities suggested in Ref.…”

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confidence: 99%

New cosmological solutions in massive gravity

et al. 2012

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We find new, simple cosmological solutions with flat, open, and closed spatial geometries, contrary to the previous wisdom that only the open model is allowed. The metric and the Stückelberg fields are given explicitly, showing nontrivial configurations of the Stückelberg in the usual FriedmannLemaître-Robertson-Walker coordinates. The solutions exhibit self-acceleration, while being free from ghost instabilities. Our solutions can accommodate inhomogeneous dust collapse represented by the Lemaître-Tolman-Bondi metric as well. Thus, our results can be used not only to describe homogeneous and isotropic cosmology but also to study gravitational collapse in massive gravity.It is very intriguing to explore whether or not the graviton can have a mass. The first attempt to add a mass term to the gravity action was made by Fierz and Pauli [1], who considered the quadratic action for the graviton h µν in flat space with the mass termThe linear theory with the Fierz-Pauli mass term is ghost-free. However, the theory does not reproduce general relativity in the massless limit m → 0. The extra three degrees of freedom in a massive spin 2 survive even in this limit, and therefore the prediction for light bending is away from that of general relativity, which clearly contradicts solar-system tests. This is called the vDVZ discontinuity [2]. As pointed out by Vainshtein [3], the discontinuity can in fact be cured by going beyond the linear theory. Massive gravity has a new length scale called the Vainshtein radius, below which the nonlinearities of the theory come in and the effect of the extra degrees of freedom is screened safely. The Vainshtein radius becomes larger as m gets smaller, and thereby a smooth massless limit is attained.However, the very nonlinearities turned out to cause another trouble. Boulware and Deser argued that there appears a sixth scalar degree of freedom at nonlinear order, which has a wrong sign kinetic term, i.e., the sixth mode is a ghost [4]. The ghost issue was emphasized in the effective field theory approach in Ref. [5]. The presence of the Boulware-Deser (BD) ghost has hindered us from constructing a consistent theory of massive gravity.Recently, a theoretical breakthrough in this field has been made. Adding higher-order self-interaction terms and tuning appropriately their coefficients, de Rham and collaborators successfully eliminated the dangerous scalar mode from the theory in the decoupling limit [6,7]. Then, Hassan and Rosen established a complete proof that the theory does not suffer from the BD ghost instability to all orders in perturbations and away from the decoupling limit [8]. Thus, there certainly exists a nonlinear theory of massive gravity that is free of the BD ghost.In addition to the theoretical interests described above, the mystery of the accelerated expansion of the Universe [9] motivates massive gravity theories as a possible alternative to dark energy. Since the attractive force mediated by a massive graviton is Yukawa-suppressed by a factor e −mr , massive gravity t...

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“…This branch is where the Schwarzschild-de Sitter solutions of [18,19] are realized (see also [20] in that context).…”

Section: Asymptotically Flat Spacetimes and The Inevitable Singularitmentioning

confidence: 99%