Black holes in a cubic Galileon universe

Babichev, Eugeny; Charmousis, Christos; Lehébel, Antoine; Moskalets, T.

doi:10.1088/1475-7516/2016/09/011

Cited by 62 publications

(106 citation statements)

References 49 publications

(87 reference statements)

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“…where a, b and c are fixed by the field equations (4.2), (4.4) and (4.5) (we omit their exact expressions here in the interest of succinctness). We note that, as was found in [20], the g(r) component of the metric is finite at the origin, unlike in GR. It is possible that this is a generic feature of any cubic Horndeski model for which such black hole solutions exist.…”

Section: Analytical Approximations In the Small And Large R Limitssupporting

confidence: 70%

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Black holes in self-tuning cubic Horndeski cosmology

2020

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Observations of neutron star mergers in the late Universe have given significant restrictions to the class of viable scalar-tensor theories. In this paper we construct black holes within the "self-tuning" class of this restricted set, whereby the bare cosmological constant is absorbed by the dynamics of the scalar, giving a lower effective cosmological constant. We use analytic expansions at the singularity, black hole and cosmological horizon, and asymptotic region, coupled with numerical solutions, to find well-behaved black holes that asymptote to the self-tuned de Sitter geometry. The geometry differs from standard general relativity black holes near the horizon, and the scalar field velocity provides a hair for the black holes.

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Section: Analytical Approximations In the Small And Large R Limitssupporting

confidence: 70%

“…Nevertheless, the problem of embedding black hole solutions in self-tuned universes has already been tackled. Such solutions have been obtained through approximate [19], numerical [20] or even exact methods [21][22][23][24]. Star solutions were also obtained numerically in similar contexts [25][26][27][28].…”

Section: Introductionmentioning

confidence: 99%

Black holes in self-tuning cubic Horndeski cosmology

2020

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“…This explains why Ref. [52] could not find simple solutions for the theory with the simplest cubic Galileon, i.e., f 3 = 1. In this case f 3 = 1, conditions (31) imply q = X 1/2 c = 0, which is inconsistent with our hypothesis of a time-dependent scalar field (34).…”

Section: B Black Hole Solutionsmentioning

confidence: 99%

Cosmological self-tuning and local solutions in generalized Horndeski theories

Babichev

Esposito-Farèse

2017

Phys. Rev. D

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We study both the cosmological self-tuning and the local predictions (inside the Solar system) of the most general shift-symmetric beyond Horndeski theory. We first show that the cosmological self-tuning is generic in this class of theories: By adjusting a mass parameter entering the action, a large bare cosmological constant can be effectively reduced to a small observed one. Requiring then that the metric should be close enough to the Schwarzschild solution in the Solar system, to pass the experimental tests of general relativity, and taking into account the renormalization of Newton's constant, we select a subclass of models which presents all desired properties: It is able to screen a big vacuum energy density, while predicting an exact Schwarzschild-de Sitter solution around a static and spherically symmetric source. As a by-product of our study, we identify a general subclass of beyond Horndeski theory for which regular self-tuning black hole solutions exist, in presence of a time-dependent scalar field. We discuss possible future development of the present work.

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“…It is worthwhile to note that through the coordinate change, the potential A μ acquires an additional component, and the first class of rotating stealth configuration (27) A way for distinguishing these two classes of solutions is to remark that the t-component of the last stealth configuration diverges at the ergosphere. Hence, it may be reasonable to consider the first configuration as the physically sound one.…”

Section: Black Hole Rotating Stealth Solutionsmentioning

confidence: 99%

“…In the past few years, Horndeski/Galileon-like theories have been extensively studied in the context of black hole physics [14][15][16][17][18][19][20][21][22][23][24][25][26][27]. In addition, solutions describing neutron stars and other compact objects have come out, imposing several constraints on the validity of these kinds of models [28][29][30][31].…”

Section: Introductionmentioning

confidence: 99%

Static and rotating solutions for vector-Galileon theories

et al. 2016

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We consider a particular truncation of the generalized Proca field theory in four dimensions for which we construct static and axisymmetric rotating black hole "stealth solutions," namely solutions with (anti) de Sitter or Kerr metric but nontrivial vector field. The static configuration is promoted to a backreacting black hole with asymptotic (anti) de Sitter behavior by turning on a nonlinear electrodynamic source given as a fixed power of the Maxwell invariant. Finally we extend our solutions to arbitrary dimensions.

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Black holes in a cubic Galileon universe

Cited by 62 publications

References 49 publications

Black holes in self-tuning cubic Horndeski cosmology

Black holes in self-tuning cubic Horndeski cosmology

Cosmological self-tuning and local solutions in generalized Horndeski theories

Static and rotating solutions for vector-Galileon theories

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