Symmetron Dark Energy in Laboratory Experiments

Upadhye, Amol

doi:10.1103/physrevlett.110.031301

Cited by 56 publications

(74 citation statements)

References 36 publications

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“…which is a solution of (3.1) and (3.2) when β c = 0 This phenomenon is similar to the one already obtained in the 1d case between infinite plates [46,48]. When m ⋆ R c ≫ 1, i.e.…”

Section: The Resonance Conditionsupporting

confidence: 86%

“…The portion of parameter space between the horizontal brown and red curves (middle and top) is excluded by the Eötwash experiment. Notice that the excluded region is a good approximation to the corresponding exclusion plot obtained using numerical simulations in [48]. The interferometry experiment excludes all the region to the left of the blue curve (leftmost one).…”

Section: Symmetronsupporting

confidence: 52%

“…Symmetrons with mass larger than the present Hubble rate are known to have relevant implications cosmologically, but cannot be tested by this method [22]. On the other hand, symmetrons with masses of order of the dark energy scale are within reach of the Eötwash types of experiments [48]. Here we find that atomic interferometry can probe symmetrons with masses a few orders of magnitude below the dark energy scale, typically with a range in vacuum smaller than a few centimeters.…”

Section: Introductionmentioning

confidence: 66%

“…For such value of µ, the Eötwash constraint applies [48] as the range is well below 6 mm, as discussed in Appendix C. These bounds are reproduced in figure (3). When the nucleus is not screened we find a bound on the parameters…”

Section: Symmetronmentioning

confidence: 82%

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Atomic interferometry test of dark energy

Brax

Davis

2016

Phys. Rev. D

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Atomic interferometry can be used to probe dark energy models coupled to matter. We consider the constraints coming from recent experimental results on models generalising the inverse power law chameleons such as f (R) gravity in the large curvature regime, the environmentally dependent dilaton and symmetrons. Using the tomographic description of these models, we find that only symmetrons with masses smaller than the dark energy scale can be efficiently tested. In this regime, the resulting constraints complement the bounds from the Eötwash experiment and exclude small values of the symmetron self-coupling.

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“…which is a solution of (3.1) and (3.2) when β c = 0 This phenomenon is similar to the one already obtained in the 1d case between infinite plates [46,48]. When m ⋆ R c ≫ 1, i.e.…”

Section: The Resonance Conditionsupporting

confidence: 86%

Section: Symmetronsupporting

confidence: 52%

Section: Introductionmentioning

confidence: 66%

Section: Symmetronmentioning

confidence: 82%

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Atomic interferometry test of dark energy

Brax

Davis

2016

Phys. Rev. D

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“…And although we have focused on chameleon searches here, there are also related laboratory signatures of symmetrons [879]. Finally, the most striking signature of chameleons can be found by testing gravity in space.…”

Section: Laboratory and Solar System Tests Of Chameleon Theoriesmentioning

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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Laboratory Constraints

Davis

Elder

2021

Modified Gravity and Cosmology

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Symmetron Dark Energy in Laboratory Experiments

Cited by 56 publications

References 36 publications

Atomic interferometry test of dark energy

Atomic interferometry test of dark energy

Beyond the cosmological standard model

Laboratory Constraints

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