Rotating boson stars in five-dimensional Einstein-Gauss-Bonnet gravity

Brihaye, Yves; Riedel, Jürgen

doi:10.1103/physrevd.89.104060

Cited by 28 publications

(30 citation statements)

References 57 publications

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“…The first step in this direction was taken in [21] with the construction of Gauss-Bonnet (GB) boson stars in asymptotically flat space-time. This was extended to rotating GB boson stars including the aAdS case [22]. In this latter paper it was conjectured that rotating GB boson stars do not exist for large values of the GB coupling.…”

Section: Introductionmentioning

confidence: 92%

Self-interacting boson stars with a single Killing vector field in anti–de Sitter space-time

2015

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We construct rotating boson stars in (4+1)-dimensional asymptotically Anti-de Sitter space-time (aAdS) with two equal angular momenta that are composed out of a massive and self-interacting scalar field. These solutions possess a single Killing vector field. We construct explicit solutions of the equations in the case of a fixed AdS background and vanishing self-coupling of the scalar field. These are the generalizations of the oscillons discussed in the literature previously now taking the mass of the scalar field into account. We study the evolution of the spectrum of massive oscillons when taking backreaction and/or the self-coupling into account numerically. We observe that very compact boson stars possess an ergoregion.

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Section: Introductionmentioning

confidence: 92%

Self-interacting boson stars with a single Killing vector field in anti–de Sitter space-time

2015

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“…Rotating boson stars in Einstein gravity show an analogue behaviour as compared to the non-rotating solutions [24,26]. In the case of rotating solutions, φ(0) = 0 and hence the derivative of φ(r) at zero, φ ′ (0), can be used as a parameter.…”

Section: Interplay Between Rotation and Gauss-bonnet Interactionmentioning

confidence: 99%

“…It was shown that the sum of the angular momenta is proportional to the Noether charge in this case. This study has been extended to include the Gauss-Bonnet (GB) interaction in [26,27] and it was shown that rotating boson stars in EGB gravity do not exist when the Gauss-Bonnet interaction dominates the gravitational interaction. Using a perturbative expansion it was shown that the solutions cease to exist in this case [27].…”

Section: Introductionmentioning

confidence: 99%

Minimal boson stars in 5 dimensions: classical instability and existence of ergoregions

Brihaye

Hartmann

2016

Class. Quantum Grav.

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We show that minimal boson stars, i.e. boson stars made out of scalar fields without self-interaction, are always classically unstable in 5 space-time dimensions. This is true for the non-rotating as well as rotating case with two equal angular momenta and in both Einstein and Gauss-Bonnet gravity, respectively, and contrasts with the 4-dimensional case, where classically stable minimal boson stars exist. We also discuss the appearance of ergoregions for rotating boson stars with two equal angular momenta. While rotating black holes typically possess an ergoregion, rotating compact objects without horizons such as boson stars have ergoregions only in a limited range of the parameter space. In this paper, we show for which values of the parameters these ergoregions appear and compare this with the case of standard Einstein gravity. We also point out that the interplay between Gauss-Bonnet gravity and rotation puts constraints on the behaviour of the space-time close to the rotation axis.

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“…The simplest case in higher dimensions is five, which has been extensively studied in several physical scenarios. We point out that the addition of the extra spatial dimension has been investigated by Kang et al [16] in static stars, Brihaye and Reidel [21] in rotating boson stars, Ghosh et al [2] in spherical collapsing bodies, and Chervon et al [22] in emergent universe models. The presence of additional dimensions may have a dramatic effect on the behaviour of matter.…”

Section: Introductionmentioning

confidence: 99%

Exact EGB models for spherical static perfect fluids

2015

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We obtain a new exact solution to the field equations for a 5-dimensional spherically symmetric static distribution in the Einstein-Gauss-Bonnet modified theory of gravity. By using a transformation, the study is reduced to the analysis of a single second order nonlinear differential equation. In general the condition of pressure isotropy produces a first order differential equation which is an Abel equation of the second kind. An exact solution is found. The solution is examined for physical admissibility. In particular a set of constants is found which ensures that a pressure-free hypersurface exists which defines the boundary of the distribution. Additionally the isotropic pressure and the energy density are shown to be positive within the radius of the sphere. The adiabatic sound-speed criterion is also satisfied within the fluid ensuring a subluminal sound speed. Furthermore, the weak, strong and dominant conditions hold throughout the distribution. On setting the Gauss-Bonnet coupling to zero, an exact solution for 5-dimensional perfect fluids in the standard Einstein theory is obtained. Plots of the dynamical quantities for the Gauss-Bonnet and the Einstein case reveal that the pressure is unaffected, while the energy density increases under the influence of the Gauss-Bonnet term.

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Rotating boson stars in five-dimensional Einstein-Gauss-Bonnet gravity

Cited by 28 publications

References 57 publications

Self-interacting boson stars with a single Killing vector field in anti–de Sitter space-time

Self-interacting boson stars with a single Killing vector field in anti–de Sitter space-time

Minimal boson stars in 5 dimensions: classical instability and existence of ergoregions

Exact EGB models for spherical static perfect fluids

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