Robinson-Trautman solution with scalar hair

Tahamtan, T.; Svítek, Otakar

doi:10.1103/physrevd.91.104032

Cited by 23 publications

(52 citation statements)

References 34 publications

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“…The relation between the asymptotic momentum and the local horizon curvature in the Robinson-Trautman class was used in the analytic explanation of an "antikick" appearing in numerical studies of an asymmetric binary black hole merger [15]. Recently, the solution with minimally coupled free scalar field was derived in [16] and shown to posses a singularity which is initially naked and only later gets covered by a horizon.…”

Section: Introductionmentioning

confidence: 99%

Robinson–Trautman solution with nonlinear electrodynamics

Tahamtan

Svítek

2016

Eur. Phys. J. C

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Explicit Robinson-Trautman solutions with an electromagnetic field satisfying nonlinear field equations are derived and analyzed. The solutions are generated from the spherically symmetric ones. In all studied cases the electromagnetic field singularity is removed while the gravitational one persists. The models resolving the curvature singularity in spherically symmetric spacetimes could not be generalized to the Robinson-Trautman geometry using the generating method developed in this paper, which indicates that the removal of a singularity in the associated spherically symmetric case might be just a consequence of high symmetry. We show that the obtained solutions are generally of algebraic type II and reduce to type D in spherical symmetry. Asymptotically they tend to the spherically symmetric case as well.

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Section: Introductionmentioning

confidence: 99%

Robinson–Trautman solution with nonlinear electrodynamics

Tahamtan

Svítek

2016

Eur. Phys. J. C

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“…In classical general relativity they were used to study counterexamples to black hole no-hair theorems or the cosmic censorship hypothesis and in many other areas. The study of scalar fields in Kundt spacetimes complements the one performed in the closely related Robinson-Trautman family [11,12].…”

Section: Introductionmentioning

confidence: 97%

“…Note that the gradient of the scalar field is now aligned with the null congruence defining the properties of spacetime (∇ μ ϕ ∝ ∂ v ), which is not possible in the case of the Robinson-Trautman family [11] where the nonzero expansion of the congruence disallows a completely aligned scalar field. Such an alignment means that scalar field propagates along this null direction and can be interpreted as a scalar wave.…”

Section: Scalar Wavesmentioning

confidence: 99%

“…In this case the Segre type is necessarily [2,11]. This means that the Ricci tensor is non-degenerate and there is no invariance group associated with it.…”

Section: Singular Modelmentioning

confidence: 99%

“…This singularity lies along the principal null direction which is at the same time the direction of propagation of gravitational waves that are present for 0 = 0 [see (35)]. This solution can be thought of as an analog of the scalar field solution in the Robinson-Trautman class given in [11].…”

Section: Conclusion and Final Remarksmentioning

confidence: 99%

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Kundt spacetimes minimally coupled to scalar field

Tahamtan

Svítek

2017

Eur. Phys. J. C

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Analytic and asymptotically flat hairy (ultra-compact) black-hole solutions and their axial perturbations

Bakopoulos

Nakas

2022

J. High Energ. Phys.

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In this work, we consider a very simple gravitational theory that contains a scalar field with its kinetic and potential terms minimally coupled to gravity, while the scalar field is assumed to have a coulombic form. In the context of this theory, we study an analytic, asymptotically flat, and regular (ultra-compact) black-hole solutions with non-trivial scalar hair of secondary type. At first, we examine the properties of the static and spherically symmetric black-hole solution — firstly appeared in [109] — and we find that in the causal region of the spacetime the stress-energy tensor, needed to support our solution, satisfies the strong energy conditions. Then, by using the slow-rotating approximation, we generalize the static solution into a slowly rotating one, and we determine explicitly its angular velocity ω(r). We also find that the angular velocity of our ultra-compact solution is always larger compared to the angular velocity of the corresponding equally massive slow-rotating Schwarzschild black hole. In addition, we investigate the axial perturbations of the derived solutions by determining the Schrödinger-like equation and the effective potential. We show that there is a region in the parameter space of the free parameters of our theory, which allows for the existence of stable ultra-compact black hole solutions. Specifically, we calculate that the most compact and stable black hole solution is 0.551 times smaller than the Schwarzschild one, while it rotates 2.491 times faster compared to the slow-rotating Schwarzschild black hole. Finally, we present without going into details the generalization of the derived asymptotically flat solutions to asymptotically (A)dS solutions.

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Robinson-Trautman solution with scalar hair

Cited by 23 publications

References 34 publications

Robinson–Trautman solution with nonlinear electrodynamics

Robinson–Trautman solution with nonlinear electrodynamics

Kundt spacetimes minimally coupled to scalar field

Analytic and asymptotically flat hairy (ultra-compact) black-hole solutions and their axial perturbations

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