Slowly rotating black hole solutions in Horndeski gravity

Maselli, Andrea; Silva, Hector O.; Minamitsuji, Masato; Berti, Emanuele

doi:10.1103/physrevd.92.104049

Cited by 90 publications

(112 citation statements)

References 56 publications

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“…Only derivatives of φ enter equations of motion. One can easily conclude from (4.19) that In the case q = q 0 , the previous expansion gets simplified as follows: 20) where Λ KGB , q 0 and Λ eff are given correspondingly in (3.6), (4.7) and (4.8), and µ is a free constant. Here we see effectively the important role played by the time dependent part of the scalar field which determines the asymptotic behavior of the black hole solution as well as the modified value of the effective cosmological constant.…”

Section: Asymptoticmentioning

confidence: 99%

Black holes in a cubic Galileon universe

Babichev

Charmousis

Lehébel

et al. 2016

J. Cosmol. Astropart. Phys.

100

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Abstract. We find and study the properties of black hole solutions for a subclass of Horndeski theory including the cubic Galileon term. The theory under study has shift symmetry but not reflection symmetry for the scalar field. The Galileon is assumed to have linear time dependence characterized by a velocity parameter. We give analytic 3-dimensional solutions that are akin to the BTZ solutions but with a non-trivial scalar field that modifies the effective cosmological constant. We then study the 4-dimensional asymptotically flat and de Sitter solutions. The latter present three different branches according to their effective cosmological constant. For two of these branches, we find families of black hole solutions, parametrized by the velocity of the scalar field. These spherically symmetric solutions, obtained numerically, are different from GR solutions close to the black hole event horizon, while they have the same de-Sitter asymptotic behavior. The velocity parameter represents black hole primary hair.arXiv:1605.07438v2 [gr-qc]

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Section: Asymptoticmentioning

confidence: 99%

Black holes in a cubic Galileon universe

Babichev

Charmousis

Lehébel

et al. 2016

J. Cosmol. Astropart. Phys.

100

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“…Clearly, the contribution to c 2 T from the two classes of operators in (2) in this case will be reduced respectively by a factor (Λ 3 /Λ) 6 and (Λ 3 /Λ) 9 . As a result, it is enough that Λ > 10 3 Λ 3 to be in agreement with observations, by which we mean not only the bound on |c 2 T − 1| but also the constraints on graviton decay [24] and dark energy instabilities induced by gravitational waves [25].…”

Section: Introduction and Setupmentioning

confidence: 93%

“…1 As a prototypical example, we will consider below the case of a linear coupling between the scalar and the Gauss-Bonnet operator, whose presence is known to be sufficient to evade the no-hair restrictions [6]. In the literature, such shift-symmetric operator has been widely studied, both analytically and numerically, in the simplest setting in which the only other operator in the Lagrangian for the scalar is the canonical kinetic term [7][8][9][10][11][12][13].…”

Section: Introduction and Setupmentioning

confidence: 99%

Black hole ringdown as a probe for dark energy

2020

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Under the assumption that a dynamical scalar field is responsible for the current acceleration of the Universe, we explore the possibility of probing its physics in black hole merger processes with gravitational wave interferometers. Remaining agnostic about the microscopic physics, we use an effective field theory approach to describe the scalar dynamics. We investigate the case in which some of the higher derivative operators, that are highly suppressed on cosmological scales, instead become important on typical distances for black holes. If a coupling to the Gauss-Bonnet operator is one of them, a non-trivial background profile for the scalar field can be sourced in the surrounding of the black hole, resulting in a potentially large amount of 'hair'. In turn, this can induce sizeable modifications to the spacetime geometry or a mixing between the scalar and the gravitational perturbations. Both effects will ultimately translate into a modification of the quasi-normal mode spectrum in a way that is also sensitive to other operators besides the one sourcing the scalar background. The presence of deviations from the predictions of general relativity in the observed spectrum can therefore serve as a window onto dark energy physics.

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“…G i = G i (φ, X ). The field equations for the metric and the scalar field stemming from the variation of (5.6) are, respectively, the following [36]:…”

Section: The Lagrangian Of Generalized Vacuum Brans-dicke Theoriesmentioning

confidence: 99%

On the action of the complete Brans–Dicke theory

Kofinas

Tsoukalas

2016

Eur. Phys. J. C

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Recently the most general completion of BransDicke theory has appeared with energy exchanged between the scalar field and ordinary matter, given that the equation of motion for the scalar field keeps the simple wave form of Brans-Dicke. This class of theories contain undetermined functions, but there exist only three theories which are unambiguously determined from consistency. Here, for the first such theory, the action of the vacuum theory is found, which arises as the limit of the full matter theory. A symmetry transformation of this vacuum action in the Jordan frame is found which consists of a conformal transformation of the metric together with a redefinition of the scalar field. Since the general family of vacuum theories is parametrized by an arbitrary function of the scalar field, the action of this family is also found. As for the full theory with matter the action of the system is only found when the matter Lagrangian vanishes on-shell, as for example for pressureless dust. Due to the interaction, the matter Lagrangian is non-minimally coupled either in the Jordan or the Einstein frame.

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Slowly rotating black hole solutions in Horndeski gravity

Cited by 90 publications

References 56 publications

Black holes in a cubic Galileon universe

Black holes in a cubic Galileon universe

Black hole ringdown as a probe for dark energy

On the action of the complete Brans–Dicke theory

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