Cosmology in rotation-invariant massive gravity with non-trivial fiducial metric

Langlois, David; Mukohyama, Shinji; Namba, Ryo; Naruko, Atsushi

doi:10.1088/0264-9381/31/17/175003

Cited by 15 publications

(41 citation statements)

References 82 publications

(214 reference statements)

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“…Further, it has been realized that the dRGT construction opens the door to building theories with multiple interacting spin-2 particles [655,658]. In what follows, we will consider Lorentz invariant theories of massive gravity, but much work has been done on Lorentz violating theories [659][660][661][662][663][664][665][666][667][668][669][670][671][672][673][674].…”

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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“…The massive gravity theory invariant under the shift symmetry φ → φ + c corresponds to b(φ) = 1. For the choice b(φ) = e Mφ , the above prescription accommodates the theory invariant under the diatonic global symmetry φ → φ + c and φ i → e −Mc φ i [76]. Besides the massive graviton potential, we also take into account the Ricci scalar R in the action and the matter field Ψ M minimally coupled to gravity.…”

Section: )mentioning

confidence: 99%

“…In Ref. [76] the authors proposed a concrete SO(3)-invariant massive gravity model with a nontrivial fiducial metric to discuss the property of de Sitter solutions. Here we will revisit them in the presence of matter and study the background dynamics relevant to the late-time cosmic acceleration.…”

Section: Flrw Background and Dark Energy Dynamicsmentioning

confidence: 99%

Dark energy survivals in massive gravity after GW170817: SO(3) invariant

Heisenberg¹,

Tsujikawa

2018

J. Cosmol. Astropart. Phys.

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The recent detection of the gravitational wave signal GW170817 together with an electromagnetic counterpart GRB 170817A from the merger of two neutron stars puts a stringent bound on the tensor propagation speed. This constraint can be automatically satisfied in the framework of massive gravity. In this work we consider a general SO(3)-invariant massive gravity with five propagating degrees of freedom and derive the conditions for the absence of ghosts and Laplacian instabilities in the presence of a matter perfect fluid on the flat Friedmann-Lemaître-Robertson-Walker (FLRW) cosmological background. The graviton potential containing the dependence of three-dimensional metrics and a fiducial metric coupled to a temporal scalar field gives rise to a scenario of the late-time cosmic acceleration in which the dark energy equation of state wDE is equivalent to −1 or varies in time. We find that the deviation from the value wDE = −1 provides important contributions to the quantities associated with the stability conditions of tensor, vector, and scalar perturbations.In concrete models, we study the dynamics of dark energy arising from the graviton potential and show that there exist viable parameter spaces in which neither ghosts nor Laplacian instabilities are present for both wDE > −1 and wDE < −1. We also generally obtain the effective gravitational coupling G eff with non-relativistic matter as well as the gravitational slip parameter ηs associated with the observations of large-scale structures and weak lensing. We show that, apart from a specific case, the two quantities G eff and ηs are similar to those in general relativity for scalar perturbations deep inside the sound horizon.

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“…Once the assumption of Lorentz-invariance is relaxed at the cosmological scale, new possibilities open up [14][15][16][17][18][19]. In particular, a massive graviton forms a representation of the three-dimensional rotation group instead of four-dimensional Lorentz group, and therefore the number of physical degrees freedom in the gravity sector does not have to be five.…”

Section: Introductionmentioning

confidence: 99%

Blue-tilted primordial gravitational waves from massive gravity

et al. 2019

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We study a theory of massive tensor gravitons which predicts blue-tilted and largely amplified primordial gravitational waves. After inflation, while their mass is significant until it diminishes to a small value, gravitons are diluted as non-relativistic matter and hence their amplitude can be substantially amplified compared to the massless gravitons which decay as radiation. We show that such gravitational waves can be detected by interferometer experiments, even if their signal is not observed on the CMB scales.

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Cosmology in rotation-invariant massive gravity with non-trivial fiducial metric

Cited by 15 publications

References 82 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

Dark energy survivals in massive gravity after GW170817: SO(3) invariant

Blue-tilted primordial gravitational waves from massive gravity

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