<i>f</i>(<i>R</i>) actions, cosmic acceleration and local tests of gravity

Navarro, Ignacio; Acoleyen, Karel Van

doi:10.1088/1475-7516/2007/02/022

Cited by 209 publications

(179 citation statements)

References 35 publications

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“…Indeed, many of the earliest studied models were ruled on out some of these grounds, with solar system constraints being the most stringent. However, classes of models were found which are compatible with solar system constraints, essentially by invoking the chameleon mechanism to screen the additional degree of freedom [274,[320][321][322][323][324][325]. The cosmologies of various models are studied in [326][327][328][329][330][331][332][333][334].…”

Section: Example: F (R) 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: Example: F (R) Gravitymentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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“…Indeed, connection to Modified Newtonian Dynamics has been made for logarithmic f (R) terms [31,32], while with other choices of f (R) connection with quintessence has been made [33][34][35][36][37][38] as well. Importantly, issues with the introduction of a "fifth force", and compatibility with terrestrial experiments have begun to be addressed through the Chameleon Effect (see [39][40][41][42] and an overview in [33]), which is used to hide the effects of field with a small mass that would otherwise be seen. It is also important to note that while f (R) theories change the action for gravity, in our approach we do not; we still take the action for gravity to be the Hilbert action with the addition of a cosmological constant.…”

Section: The F (R) Theorymentioning

confidence: 99%

Dark energy and extending the geodesic equations of motion: its construction and experimental constraints

Speliotopoulos

2010

Gen Relativ Gravit

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With the discovery of Dark Energy, DE , there is now a universal length scale, DE = c/( DE G) 1/2 , associated with the universe that allows for an extension of the geodesic equations of motion. In this paper, we will study a specific class of such extensions, and show that contrary to expectations, they are not automatically ruled out by either theoretical considerations or experimental constraints. In particular, we show that while these extensions affect the motion of massive particles, the motion of massless particles are not changed; such phenomena as gravitational lensing remain unchanged. We also show that these extensions do not violate the equivalence principal, and that because DE = 14010 800 820 Mpc, a specific choice of this extension can be made so that effects of this extension are not be measurable either from terrestrial experiments, or through observations of the motion of solar system bodies. A lower bound for the only parameter used in this extension is set.

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“…The f R field is massive, and below its Compton wavelength, it enhances gravitational forces by a factor of 1/3, increasing the growth of structure. Due to the density dependence of the scalaron's mass, f (R) gravity models may incorporate the chameleon suppression [8][9][10], returning gravitational forces to Newtonian relations in high-density regions and making them compatible with Solar System tests [11,12].…”

Section: Introductionmentioning

confidence: 99%

Modeling halo mass functions in chameleonf(R)gravity

et al. 2013

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On cosmological scales, observations of the cluster abundance currently place the strongest constraints on f (R) gravity. These constraints lie in the large-field limit, where the modifications of general relativity can correctly be modeled by setting the Compton wavelength of the scalar field to its background value. These bounds are, however, at the verge of penetrating into a regime where the modifications become nonlinearly suppressed due to the chameleon mechanism and cannot be described by this linearized approximation. For future constraints based on observations subjected to cluster abundance, it is therefore essential to consistently model the chameleon effect. We analyze descriptions of the halo mass function in chameleon f (R) gravity using a mass-and environmentdependent spherical collapse model in combination with excursion set theory and phenomenological fits to N -body simulations in the ΛCDM and f (R) gravity scenarios. Our halo mass functions consistently incorporate the chameleon suppression and cosmological parameter dependencies, improving upon previous formalisms and providing an important extension to N -body simulations for the application in consistent tests of gravity with observables sensitive to the abundance of clusters.

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f(R) actions, cosmic acceleration and local tests of gravity

Cited by 209 publications

References 35 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

Dark energy and extending the geodesic equations of motion: its construction and experimental constraints

Modeling halo mass functions in chameleonf(R)gravity

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