PAIR OF ACCELERATED BLACK HOLES IN AN ANTI-DE SITTER BACKGROUND: THE ADS <font>C</font>-METRIC

Dias, Óscar J. C.; Lemos, José P. S.

doi:10.1142/9789812791160_0025

Cited by 41 publications

(131 citation statements)

References 31 publications

(93 reference statements)

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“…A natural question at this stage is whether the results of this paper would apply to other generalisations of the C-metric, such as the de Sitter / anti-de Sitter C-metric [5,17,18,19] or the rotating C-metric [5,12,20]. In the latter case, while it is straightforward to write down a form for it which has a naturally factorisable structure function, this form cannot be obtained from the usual form of the rotating C-metric by a coordinate transformation.…”

Section: Discussionmentioning

confidence: 99%

A new form of the C-metric

Hong

Teo

2003

Class. Quantum Grav.

125

182

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The usual form of the C-metric has the structure function G(ξ) = 1 − ξ 2 − 2mAξ 3 , whose cubic nature can make calculations cumbersome, especially when explicit expressions for its roots are required. In this paper, we propose a new form of the C-metric, with the explicitly factorisable structure function G(ξ) = (1 − ξ 2 )(1 + 2mAξ). Although this form is related to the usual one by a coordinate transformation, it has the advantage that its roots are now trivial to write down. We show that this leads to potential simplifications, for example, when casting the C-metric in Weyl coordinates. These results also extend to the charged C-metric, whose structure function can be written in the new formwhere r ± are the usual locations of the horizons in the Reissner-Nordström solution. As a by-product, we explicitly cast the extremally charged C-metric in Weyl coordinates.

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Section: Discussionmentioning

confidence: 99%

A new form of the C-metric

Hong

Teo

2003

Class. Quantum Grav.

125

182

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“…Further properties of the charged C-metric in a (anti-)de Sitter background have been analysed in [17] and [33]- [36]. However, these worked with a different form of the metric to that above.…”

Section: The Chargedmentioning

confidence: 99%

A New Look at the Plebański–demiański Family of Solutions

Griffiths

Podolský

2006

Int. J. Mod. Phys. D

237

321

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The Plebański-Demiański metric, and those that can be obtained from it by taking coordinate transformations in certain limits, include the complete family of space-times of type D with an aligned electromagnetic field and a possibly non-zero cosmological constant. Starting with a new form of the line element which is better suited both for physical interpretation and for identifying different subfamilies, we review this entire family of solutions. Our metric for the expanding case explicitly includes two parameters which represent the acceleration of the sources and the twist of the repeated principal null congruences, the twist being directly related to both the angular velocity of the sources and their NUT-like properties. The nonexpanding type D solutions are also identified. All special cases are derived in a simple and transparent way.

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“…[7,83,109,110] for reviews and references) to admit a cosmological constant [111][112][113][114][115]. For Λ > 0 it represents a pair of uniformly accelerated possibly charged black holes in de Sitterlike universe.…”

Section: On Studies Of Asymptotic Behaviour Of Radiative Fields In Gementioning

confidence: 99%

Asymptotic directional structure of radiative fields in spacetimes with a cosmological constant

Krtouš¹,

Podolský²

2004

Class. Quantum Grav.

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Abstract. We analyze the directional properties of general gravitational, electromagnetic, and spin-s fields near conformal infinity I. The fields are evaluated in normalized tetrads which are parallelly propagated along null geodesics which approach a point P of I. The standard peelingoff property is recovered and its meaning is discussed and refined. When the (local) character of the conformal infinity is null, such as in asymptotically flat spacetimes, the dominant term which is identified with radiation is unique. However, for spacetimes with a non-vanishing cosmological constant the conformal infinity is spacelike (for Λ > 0) or timelike (for Λ < 0), and the radiative component of each field depends substantially on the null direction along which P is approached.The directional dependence of asymptotic fields near such de Sitter-like or anti-de Sitterlike I is explicitly found and described. We demonstrate that the corresponding directional structure of radiation has a universal character that is determined by the algebraic (Petrov) type of the field. In particular, when Λ > 0 the radiation vanishes only along directions which are opposite to principal null directions. For Λ < 0 the directional dependence is more complicated because it is necessary to distinguish outgoing and ingoing radiation. Near such anti-de Sitterlike conformal infinity the corresponding directional structures differ, depending not only on the number and degeneracy of the principal null directions at P but also on their specific orientation with respect to I.The directional structure of radiation near (anti-)de Sitter-like infinities supplements the standard peeling-off property of spin-s fields. This characterization offers a better understanding of the asymptotic behaviour of the fields near conformal infinity under the presence of a cosmological constant.

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PAIR OF ACCELERATED BLACK HOLES IN AN ANTI-DE SITTER BACKGROUND: THE ADS C-METRIC

Cited by 41 publications

References 31 publications

A new form of the C-metric

A new form of the C-metric

A New Look at the Plebański–demiański Family of Solutions

Asymptotic directional structure of radiative fields in spacetimes with a cosmological constant

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