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Neutron star sensitivities in Hořava gravity after GW170817

Physical review. D, Particles, fields, gravitation, and cosmology, 2019-10, Vol.100 (8) [Peer Reviewed Journal]

Distributed under a Creative Commons Attribution 4.0 International License ;ISSN: 1550-7998 ;EISSN: 1550-2368 ;DOI: 10.1103/PhysRevD.100.084053

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  • Title:
    Neutron star sensitivities in Hořava gravity after GW170817
  • Author: Barausse, Enrico
  • Subjects: Astrophysics ; Sciences of the Universe
  • Is Part Of: Physical review. D, Particles, fields, gravitation, and cosmology, 2019-10, Vol.100 (8)
  • Description: 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 bound 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 nonpathological 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 at the leading post-Newtonian order, 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.
  • Publisher: American Physical Society
  • Language: English
  • Identifier: ISSN: 1550-7998
    EISSN: 1550-2368
    DOI: 10.1103/PhysRevD.100.084053
  • Source: Hyper Article en Ligne (HAL) (Open Access)
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