Hořava gravity after GW170817

Gümrükçüoğlu, A. Emir; Saravani, Mehdi; Sotiriou, Thomas P.

doi:10.1103/physrevd.97.024032

Cited by 114 publications

(135 citation statements)

References 56 publications

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“…This bounds one of the parameters of the theory, β, to |β| 10 −15 [34,35]. Further bounds follow from combining the GW170817/GRB 170817A observations with solar system constraints on the preferred frame parameters [34,35]. Indeed, if one imposes |β| 10 −15 , the latter are satisfied by |α| < ∼ 10 −7 , at least if |λ| ≫ 10 −7 ; or by |α| < ∼ 0.25 × 10 −4 and λ ≈ α/(1−2α) [35].…”

Section: Introductionmentioning

confidence: 97%

“…More recently, the coincident gravitational wave and electromagnetic detection of GW170817 and GRB 170817A [31,32] has constrained the propagation speeds of gravitational waves and light to match to within a part in 10 15 [33]. This bounds one of the parameters of the theory, β, to |β| 10 −15 [34,35]. Further bounds follow from combining the GW170817/GRB 170817A observations with solar system constraints on the preferred frame parameters [34,35].…”

Section: Introductionmentioning

confidence: 99%

“…This second possibility implies small values for all three coupling constants (|α| ∼ |λ| 10 −5 and |β| 10 −15 ), while the first tightly constrains α and β (|α| < ∼ 10 −7 , |β| < ∼ 10 −15 ) but leaves λ essentially unconstrained. The only bounds on λ are then λ 0.01 − 0.1, from measurements of the abundance of primordial elements produced during Big Bang Nucleosynthesis [28][29][30] and from Cosmic Microwave Background observations [36]; and the sign requirement λ ≥ 0 needed to ensure the absence of ghosts [12,34]. In the light of these constraints, it is therefore quite tempting to simply set α and β exactly to zero while keeping λ finite.…”

Section: Introductionmentioning

confidence: 99%

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Neutron star sensitivities in Hořava gravity after GW170817

Barausse

2019

Phys. Rev. D

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Hořava gravity breaks boost invariance in the gravitational sector by introducing a preferred time foliation. The dynamics of this preferred slicing is governed, in the low-energy limit suitable for most astrophysical applications, by three dimensionless parameters α, β and λ. The first two of these parameters are tightly bounded by solar system and gravitational wave propagation experiments, but λ remains relatively unconstrained (0 ≤ λ 0.01 − 0.1). We restrict here to the parameter space region defined by α = β = 0 (with λ kept generic), which in a previous paper we showed to be the only one where black hole solutions are non-pathological at the universal horizon, and we focus on possible violations of the strong equivalence principle in systems involving neutron stars. We compute neutron star "sensitivities", which parametrize violations of the strong equivalence principle, and find that they vanish identically, like in the black hole case, for α = β = 0 and generic λ = 0. This implies that no violations of the strong equivalence principle (neither in the conservative sector nor in gravitational wave fluxes) can occur at the leading post-Newtonian order in binaries of compact objects, and that data from binary pulsars and gravitational interferometers are unlikely to further constrain λ.

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Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Neutron star sensitivities in Hořava gravity after GW170817

Barausse

2019

Phys. Rev. D

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“…In the IR, the theory reduces to that of general rela-tivity. Much work has been done on this theory, including some early contributions to cure some of the original inconsistencies [7][8][9]11,12,14,18,19,21,[38][39][40][41][42][43][44][45]. The presence of the anisotropic scaling in the theory leads to a natural description using the Arnowit-Deser-Misner (ADM) formulation, in which the metric reads:…”

Section: Hořava-lifshitz Gravitymentioning

confidence: 99%

Preferred-frame effects, the $$H_0$$ tension, and probes of Hořava–Lifshitz gravity

Nilsson

2020

Eur. Phys. J. Plus

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We discuss implications on the H 0 tension due to preferred-frame effects in the context of Hořava-Lifshitz gravity. By using a combination of lowredshift data (Sne1a, elliptical and lenticular galaxies, GRB's, and quasars) we discuss the H 0 tension and its appearance as a preferred-frame effect, as well as present new constraints on the model parameter λ. Moreover, from the structure of the Friedmann equations, we argue that up to 36% of the Hubble tension can be explained by Lorentz-violating effects in a Hořava-Lifshitz scenario.

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“…KAGRA [13,14] has now joint LIGO/Virgo network, and their observations might put stronger constraint on the GW polarization content. Moreover, the measurement of the GW speed from GW170817 and GRB 170817A [5,[15][16][17] has already severally constrained some of the alternatives [11,[18][19][20][21][22][23][24][25]. With the advent of the space-borne and more advanced 3rd generation detectors such as Einstein Telescope [26], more GW events can be detected, and our understanding of the nature of gravity, and thereby other phenomena such as the cosmology, can be greatly improved.…”

Section: Introductionmentioning

confidence: 99%

Corrections to the gravitational wave phasing

2020

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The gravitational wave, traveling a long cosmological distance to reach the interferometers, interacts with the cosmological background, so generally speaking, its amplitude and phase are modified in some nontrivial way. As the sensitivity of the interferometers are improved, one may detect the corrections to the short-wavelength approximation, which naturally includes the information of the cosmological evolution. In this work, the calculation of the Newman-Penrose variable Ψ4 has been done to show that there are two new corrections to the short-wavelength approximation. One formally occurs at the 1st post-Newtonian order, but is highly suppressed by the Hubble parameters; the other occurs at the 5th post-Newtonian order, which is due to the variation of the amplitude. The first correction contains the evolution of the universe, but it may not be easily detected. The second one indicates that the short-wavelength approximation has to be corrected, when the more accurate waveforms with the higher order post-Newtonian terms are calculated.

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Hořava gravity after GW170817

Abstract: The recent detection of gravitational wave GW170817 has placed a severe bound on the deviation of the speed of gravitational waves from the speed of light. We explore the consequences of this detection for Hořava gravity.

Cited by 114 publications

References 56 publications

Neutron star sensitivities in Hořava gravity after GW170817

Neutron star sensitivities in Hořava gravity after GW170817

Preferred-frame effects, the $$H_0$$ tension, and probes of Hořava–Lifshitz gravity

Corrections to the gravitational wave phasing

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