Strong interactions and exact solutions in nonlinear massive gravity

Koyama, K.; Niz, Gustavo; Tasinato, Gianmassimo

doi:10.1103/physrevd.84.064033

Cited by 217 publications

(248 citation statements)

References 41 publications

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“…As a result, the theory exhibits two classes of static spherically symmetric solutions, which differ in how the scalar sector couples to graviton. The first class of solutions naturally contains (Anti) de Sitter-Schwarzschild solutions, where the cosmological constant is proportional to the graviton's mass [7,8,9]. Some of these solutions are very similar to those found many years ago in the simple Fierz-Pauli model [10], and what characterises them is that the scalar mode is strongly coupled everywhere, which avoids a discontinuous connection to GR in the massless limit.…”

Section: Introductionmentioning

confidence: 73%

“…Therefore, it is imperative to include non-linearities in the scalar sector in order to study the Vainshtein mechanism. Solutions presenting these behaviour in massive gravity where found in [15], and more recently in the ghost-free model considered here in [7,8,17,18]. Unfortunately, these solutions do not cover the whole parameter space of the theory as we will describe here.…”

Section: Introductionmentioning

confidence: 97%

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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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Section: Introductionmentioning

confidence: 73%

Section: Introductionmentioning

confidence: 97%

Characterizing Vainshtein solutions in massive gravity

Sbisà

Niz

Koyama³

et al. 2012

Phys. Rev. D

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“…For instance, there are such known solutions [13,[34][35][36][37][38][39], where the background dynamics is FLRW-like (or reduces to FLRW through cosmological Vainshtein mechanism [13]) while the Stückelberg sector is contaminated by spatial inhomogeneities. In principle, these may also evade the FLRW ghost, although in the lack of symmetry, the stability analysis of perturbations becomes technically challenging (although see [40]).…”

Section: Discussionmentioning

confidence: 99%

Nonlinear stability of cosmological solutions in massive gravity

Felice

Gümrükçüoğlu

Lin

et al. 2013

J. Cosmol. Astropart. Phys.

106

100

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We investigate nonlinear stability of two classes of cosmological solutions in massive gravity: isotropic Friedmann-Lemaître-Robertson-Walker (FLRW) solutions and anisotropic FLRW solutions. For this purpose we construct the linear cosmological perturbation theory around axisymmetric Bianchi type-I backgrounds. We then expand the background around the two classes of solutions, which are fixed points of the background evolution equation, and analyze linear perturbations on top of it. This provides a consistent truncation of nonlinear perturbations around these fixed point solutions and allows us to analyze nonlinear stability in a simple way. In particular, it is shown that isotropic FLRW solutions exhibit nonlinear ghost instability. On the other hand, anisotropic FLRW solutions are shown to be ghost-free for a range of parameters and initial conditions.

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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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Strong interactions and exact solutions in nonlinear massive gravity

Cited by 217 publications

References 41 publications

Characterizing Vainshtein solutions in massive gravity

Characterizing Vainshtein solutions in massive gravity

Nonlinear stability of cosmological solutions in massive gravity

Beyond the cosmological standard model

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