Axial quasinormal modes of Einstein-Gauss-Bonnet-dilaton neutron stars

Blázquez-Salcedo, Jose Luis; González-Romero, L. M.; Kunz, Jutta; Mojica, Sindy; Navarro‐Lérida, Francisco

doi:10.1103/physrevd.93.024052

Cited by 37 publications

(36 citation statements)

References 45 publications

(78 reference statements)

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“…Since both EOSs do not yield a maximum mass of 2M ⊙ in the static case and for slow rotation, the present studies should be extended to investigate further EOSs, yielding higher masses. In the static case, this has already been achieved in [23] for a set of eight realistic EOSs. For the rapidly rotating case, however, the current numerical scheme will need to be revised first in order to achieve higher efficiency.…”

Section: Discussionmentioning

confidence: 92%

“…Note, that in [23] a set of eight realistic EOSs was employed to obtain sequences of static neutron stars in dEGB theory and to study the effect of the dilaton and the GB term.…”

Section: B Equations Of Statementioning

confidence: 99%

“…There it was shown that the moment of inertia decreases with increasing GB coupling. Recently, also QNMs of neutron stars were studied in dEGB theory [23], showing that the frequency of the modes is increased by the presence of the GB term.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 92%

“…Note, that in [23] a set of eight realistic EOSs was employed to obtain sequences of static neutron stars in dEGB theory and to study the effect of the dilaton and the GB term.…”

Section: B Equations Of Statementioning

confidence: 99%

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

et al. 2016

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“…However these attempts are usually limited to spherical symmetry, and they often lead to the conclusion that large classes of black hole solutions are unstable [27,28]. As far as we know, QNM frequencies in modified gravity were computed only in a handful of cases, specifically in Einstein-dilaton-Gauss-Bonnet [29][30][31] and dynamical Chern-Simons [32,33] theories, and even then only for spherically symmetric black hole solutions. These calculations are therefore of limited utility in data analysis applications, both because they must be developed on a case-by-case basis, and because the remnant of a binary black hole merger is almost inevitably a rotating black hole 1 .…”

Section: A the Eikonal Post-kerr Parametrization Schemementioning

confidence: 99%

Post-Kerr black hole spectroscopy

et al. 2017

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One of the central goals of the newborn field of gravitational wave astronomy is to test gravity in the highly nonlinear, strong field regime characterizing the spacetime of black holes. In particular, "black hole spectroscopy" (the observation and identification of black hole quasinormal mode frequencies in the gravitational wave signal) is expected to become one of the main tools for probing the structure and dynamics of Kerr black holes. In this paper we take a significant step towards that goal by constructing a "post-Kerr" quasinormal mode formalism. The formalism incorporates a parametrized but general perturbative deviation from the Kerr metric and exploits the well-established connection between the properties of the spacetime's circular null geodesics and the fundamental quasinormal mode to provide approximate, eikonal limit formulae for the modes' complex frequencies. The resulting algebraic toolkit can be used in waveform templates for ringing black holes with the purpose of measuring deviations from the Kerr metric. As a first illustrative application of our framework, we consider the Johannsen-Psaltis deformed Kerr metric and compute the resulting deviation in the quasinormal mode frequency relative to the known Kerr result.

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“…While their axial oscillations have been studied in [10]. Rapidly rotating * Electronic address: kostas.kokkotas@uni-tuebingen.de † Electronic address: roman.konoplya@uni-tuebingen.de ‡ Electronic address: olexandr.zhydenko@ufabc.edu.br neutron star models were also constructed in EdGB gravity [11,12].…”

Section: Introductionmentioning

confidence: 99%

Analytical approximation for the Einstein-dilaton-Gauss-Bonnet black hole metric

2017

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We construct an analytical approximation for the numerical black hole metric of P. Kanti, et. al. [Phys. Rev. D 54, 5049 (1996)] in the four-dimensional Einstein-dilaton-Gauss-Bonnet (EdGB) theory. The continued fraction expansion in terms of a compactified radial coordinate, used here, converges slowly when the dilaton coupling approaches its extremal values, but for a black hole far from the extremal state, the analytical formula has a maximal relative error of a fraction of one percent already within the third order of the continued fraction expansion. The suggested analytical representation of the numerical black hole metric is relatively compact and good approximation in the whole space outside the black hole event horizon. Therefore, it can serve in the same way as an exact solution when analyzing particles' motion, perturbations, quasinormal modes, Hawking radiation, accreting disks and many other problems in the vicinity of a black hole. In addition, we construct the approximate analytical expression for the dilaton field.

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Axial quasinormal modes of Einstein-Gauss-Bonnet-dilaton neutron stars

Cited by 37 publications

References 45 publications

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

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

Post-Kerr black hole spectroscopy

Analytical approximation for the Einstein-dilaton-Gauss-Bonnet black hole metric

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