Erratum: Constraints on Einstein-Æther theory and Hořava gravity from binary pulsar observations [Phys. Rev. D<b>89</b>, 084067 (2014)]

Yagi, Kent; Blas, Diego; Barausse, Enrico; Yunes, Nicolás

doi:10.1103/physrevd.90.069902

Cited by 95 publications

(212 citation statements)

References 0 publications

Supporting

Mentioning

207

Contrasting

Order By: Relevance

“…Including tidal effects in pointparticle templates calibrated to highly accurate BH-BH waveforms from NR (e.g., EOB waveforms) is the best way of controlling systematic errors due to lack of knowledge of higher-order point-particle terms in the PN expansion. In fact, employing inspiraling, point-particle PN templates augmented by tidal effects, leads to large systematic biases and limits the extraction of tidal information [418,419].…”

Section: Challengesmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

View full text Add to dashboard Cite

Section: Challengesmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

View full text Add to dashboard Cite

“…This generalizes similar expressions for scalar-tensor theories [17], and Lorentz-violating gravity [10,11]. Let us now consider an action depending also on second derivatives of the metric and extra gravitational degrees of freedom φ A (e.g.…”

mentioning

confidence: 99%

“…Here, we generalize previous work in scalar-tensor theories [17,18] and Lorentz-violating gravity [10,11] by introducing a formalism to calculate the sensitivities of stars (including pulsars) in generic theories. As an application, we calculate them in the most general scalar-tensor theories ("Horndeski theories" or "generalized galileons") [19][20][21] that have second-order field equations and are invariant under a shift of the scalar field φ, i.e.…”

mentioning

confidence: 99%

“…Therefore, knowledge of the sensitivities is crucial to verify the agreement between a theory and GW observations (binary-pulsar data or direct detections). For example, binary pulsars have already placed strong constraints on Lorentz-symmetry violations in gravity [10,11] and on certain scalar-tensor theories [8,12,13], and even stronger bounds will be possible with direct GW detections [14][15][16].…”

mentioning

confidence: 99%

See 1 more Smart Citation

Gravitation-Wave Emission in Shift-Symmetric Horndeski Theories

Barausse

Yagi

2015

Phys. Rev. Lett.

Self Cite

View full text Add to dashboard Cite

Gravity theories beyond General Relativity typically predict dipolar gravitational emission by compact-star binaries. This emission is sourced by "sensitivity" parameters depending on the stellar compactness. We introduce a general formalism to calculate these parameters, and show that in shift-symmetric Horndeski theories stellar sensitivities and dipolar radiation vanish, provided that the binary's dynamics is perturbative (i.e. the post-Newtonian formalism is applicable) and cosmological-expansion effects can be neglected. This allows reproducing the binary-pulsar observed orbital decay.

show abstract

“…Now, for η → 2ξ, it reduces to a constant, μ un ¼ 16H 2 0 . On top of these theoretical considerations one may want to consider additional constraints coming from PPN, binary pulsars or Cherenkov radiation [51]. Such additional constraints are complementary to the ones obtained in our paper and in the case that these have to be imposed, our results ensure that the theory is stable.…”

Section: B Low-energy Hořava Gravitymentioning

confidence: 51%

de Sitter limit analysis for dark energy and modified gravity models

2017

View full text Add to dashboard Cite

The effective field theory of dark energy and modified gravity is supposed to well describe, at low energies, the behavior of the gravity modifications due to one extra scalar degree of freedom. The usual curvature perturbation is very useful when studying the conditions for the avoidance of ghost instabilities as well as the positivity of the squared speeds of propagation for both the scalar and tensor modes, or the Stückelberg field performs perfectly when investigating the evolution of linear perturbations. We show that the viable parameter space identified by requiring no-ghost instabilities and positive squared speeds of propagation does not change by performing a field redefinition, while the requirement of the avoidance of tachyonic instability might instead be different. Therefore, we find it interesting to associate to the general modified gravity theory described in the effective field theory framework, a perturbation field which will inherit all of the properties of the theory. In the present paper we address the following questions: (1) how can we define such a field? and (2) what is the mass of such a field as the background approaches a final de Sitter state? We define a gauge-invariant quantity which identifies the density of the dark energy perturbation field valid for any background. We derive the mass associated to the gauge-invariant dark energy field on a de Sitter background, which we retain to be still a good approximation also at very low redshift (z ≃ 0). On this background we also investigate the value of the speed of propagation and we find that there exist classes of theories which admit a nonvanishing speed of propagation, even in the Horndeski model, for which a zero speed of sound has previously been found in the literature. We finally apply our results to specific well-known models.

show abstract

Erratum: Constraints on Einstein-Æther theory and Hořava gravity from binary pulsar observations [Phys. Rev. D89, 084067 (2014)]

Cited by 95 publications

References 0 publications

Sources of Gravitational Waves: Theory and Observations

Sources of Gravitational Waves: Theory and Observations

Gravitation-Wave Emission in Shift-Symmetric Horndeski Theories

de Sitter limit analysis for dark energy and modified gravity models

Contact Info

Product

Resources

About