Class of Stationary Axisymmetric Solutions of the Einstein-Maxwell-Dilaton-Axion Field Equations

Garcı́a, Alberto; Gal’tsov, D.V.; Kechkin, Oleg V.

doi:10.1103/physrevlett.74.1276

Cited by 131 publications

(101 citation statements)

References 10 publications

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“…As another test of the convergence properties of our metric parametrization we next consider a dilaton-axion black hole [14]. When both the axion field and the spin vanish, such a black hole is described by a spherically symmetric metric with line element…”

Section: Parametrization For Dilaton Black Holesmentioning

confidence: 99%

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New parametrization for spherically symmetric black holes in metric theories of gravity

2014

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We propose a new parametric framework to describe in generic metric theories of gravity the spacetime of spherically symmetric and slowly rotating black holes. In contrast to similar approaches proposed so far, we do not use a Taylor expansion in powers of M=r, where M and r are the mass of the black hole and a generic radial coordinate, respectively. Rather, we use a continued-fraction expansion in terms of a compactified radial coordinate. This choice leads to superior convergence properties and allows us to approximate a number of known metric theories with a much smaller set of coefficients. The measure of these coefficients via observations of near-horizon processes can be used to effectively constrain and compare arbitrary metric theories of gravity. Although our attention is here focussed on spherically symmetric black holes, we also discuss how our approach could be extended to rotating black holes.

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Section: Parametrization For Dilaton Black Holesmentioning

confidence: 99%

“…However, if we assume that the function ω depends on the radial coordinate r only, then we obtain a metric which can be associated with a slowly rotating black hole in Hořava-Lifshitz theory [25], in Einstein-aether gravity [26], in Chern-Simons modified gravity [27], or with dilatonic Einstein-GaussBonnet [28] and dilaton-axion black holes [14].…”

mentioning

confidence: 99%

New parametrization for spherically symmetric black holes in metric theories of gravity

2014

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“…[37][38][39][40][41][42][43][44][45][46][47][48]), as well as rapidly rotating ones (see e.g. [49][50][51][52][53]). Also string theory corrections of further compact objects have been considered (see e.g.…”

Section: A Action and Field Equationsmentioning

confidence: 99%

Rapidly rotating neutron stars in dilatonic Einstein-Gauss-Bonnet theory

et al. 2016

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We construct sequences of rapidly rotating neutron stars in dilatonic Einstein-Gauss-Bonnet theory, employing two equations of state for the nuclear matter. We analyze the dependence of the physical properties of these neutron stars on the Gauss-Bonnet coupling strength. For a given equation of state we determine the physically relevant domain of rapidly rotating neutron stars, which is delimited by the set of neutron stars rotating at the Kepler limit, the set of neutron stars along the secular instability line, and the set of static neutron stars. As compared to Einstein gravity, the presence of the Gauss-Bonnet term decreases this domain, leading to lower values for the maximum mass as well as to smaller central densities. The quadrupole moment is decreased by the GaussBonnet term for rapidly rotating neutron stars, while it is increased for slowly rotating neutron stars. The universal relation between the quadrupole moment and the moment of inertia found in General Relativity appears to extend to dilatonic Einstein-Gauss-Bonnet theory with very little dependence on the coupling strength of the Gauss-Bonnet term. The neutron stars carry a small dilaton charge.

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“…These conditions lead to a unique choice of the restriction: P 1 = Q 1 = 0 and arbitrary values for the remaining parameters P 2 , Q 2 and Q 3 . In this special case the calculation of the scalar potentials becomes much simpler and one finally obtains S 0 = 1 and 10) where now τ = −P . Note that the parameter P 2 can be removed from Eqs.…”

Section: Explicit Solutions Via 3d Dilaton Gravitymentioning

confidence: 99%

“…The class of extremal Israel-Wilson-Perjes solutions arises when the (numerical) parameter κ, defined by the relation 10) vanishes, the dynamical quantity Λ is harmonic and the three-metric h µν is flat. In the Einstein-Maxwell theory the situation is extremely similar to this one according to the correspondence rule (3.5): the ansatz z = λq, where λ is a complex function and q is a 1 × 2 constant complex parameter, gives the conventional Israel-Wilson-Perjes class of solutions if the parameter κ = qσ 3 q + iz zero, λ is harmonic and the three-metric is again flat.…”

Section: String Theories From Static Einstein-maxwell Systemmentioning

confidence: 99%

String Theory Extensions of Einstein–maxwell Fields: The Static Case

Herrera–Aguilar

Kechkin

2002

Int. J. Mod. Phys. A

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We present a new approach for generating solutions in both the four-dimensional heterotic string theory with one vector field and the five-dimensional bosonic string theory, starting from static Einstein-Maxwell fields. Our approach allows one to construct classes of solutions which are invariant with respect to the total subgroup of three-dimensional charging symmetries of these string theories. The new solutiongenerating procedure leads to the extremal Israel-Wilson-Perjes subclass of string theory solutions in a special case and provides its natural continuous extension to the realm of non-extremal solutions. We explicitly calculate all string theory solutions related to three-dimensional gravity coupled to an effective dilaton field which arises after an appropriate charging symmetry invariant reduction of the static Einstein-Maxwell system.

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Class of Stationary Axisymmetric Solutions of the Einstein-Maxwell-Dilaton-Axion Field Equations

Cited by 131 publications

References 10 publications

New parametrization for spherically symmetric black holes in metric theories of gravity

New parametrization for spherically symmetric black holes in metric theories of gravity

Rapidly rotating neutron stars in dilatonic Einstein-Gauss-Bonnet theory

String Theory Extensions of Einstein–maxwell Fields: The Static Case

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