Constraints on Einstein-dilation-Gauss-Bonnet gravity from Black Hole-Neutron Star Gravitational Wave Events

Lyu, Zhenwei; Jiang, Nan; Yagi, Kent

doi:10.48550/arxiv.2201.02543

Cited by 5 publications

(16 citation statements)

References 71 publications

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“…( 13)] available online [82]. However, near the saturation of the bound (12), i.e., when 2 = 1 − 24 4…”

Section: B Nonrotating Black Holesmentioning

confidence: 99%

“…Given these results, it is not clear that a naked singularity arises when one saturates the bound in Eq. (12) (see e.g. [29,35]).…”

Section: A Shift-symmetric Theorymentioning

confidence: 99%

“…( 9) outwards, from r * = r/r H = 1 up to a large value of r * , and we extract the asymptotic scalar field value φ. We repeat these steps for a range of ϕ H values allowed by the reality condition (12), while keeping * fixed. The outcome is a function φ(ϕ H ) that generally has a single zero at ϕ H = 0 corresponding to the Schwarzschild solution [cf.…”

Section: Appendix C: Black Hole Sensitivity βmentioning

confidence: 99%

“…The detection of gravitational waves from compact binary coalescences by the LIGO-Virgo collaboration [1][2][3] started a new era in experimental gravitational physics where, for the first time, we can test the predictions of general relativity (and modifications thereof) in highly dynamical, nonlinear environments [4][5][6][7][8][9][10][11][12]. A prerequisite to perform such tests is a description of the orbital dynamics and the associated gravitational wave emission of inspiralling compact objects (i.e., neutron stars and black holes) in relativistic gravity theories [13][14][15].…”

Section: Introductionmentioning

confidence: 99%

“…As a consequence, black holes are endowed with a monopole scalar charge, which can source dipolar scalar radiation in binary black hole systems [43,44]. This makes black hole binaries ideal systems to constrain (or to look for evidence in favor of) these theories with current [10][11][12] and future gravitational-wave observatories [45,46].…”

Section: Introductionmentioning

confidence: 99%

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Black hole sensitivities in Einstein-scalar-Gauss-Bonnet gravity

Julié,

Silva,

Berti

et al. 2022

Preprint

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The post-Newtonian dynamics of black hole binaries in Einstein-scalar-Gauss-Bonnet theories of gravity depends on the so-called "sensitivities", quantities which characterize a black hole's adiabatic response to the time-dependent scalar field environment sourced by its companion. In this work, we calculate numerically the sensitivities of nonrotating black holes, including spontaneously scalarized ones, in three classes of Einstein-scalar-Gauss-Bonnet gravity: the shift-symmetric, dilatonic and Gaussian theories. When possible, we compare our results against perturbative analytical results, finding excellent agreement. Unlike their general relativistic counterparts, black holes in Einsteinscalar-Gauss-Bonnet gravity only exist in a restricted parameter space controlled by the theory's coupling constant. A preliminary study of the role played by the sensitivities in black hole binaries suggests that, in principle, black holes can be driven outside of their domain of existence during the inspiral, for binary parameters which we determine.

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“…( 13)] available online [82]. However, near the saturation of the bound (12), i.e., when 2 = 1 − 24 4…”

Section: B Nonrotating Black Holesmentioning

confidence: 99%

“…Given these results, it is not clear that a naked singularity arises when one saturates the bound in Eq. (12) (see e.g. [29,35]).…”

Section: A Shift-symmetric Theorymentioning

confidence: 99%

Section: Appendix C: Black Hole Sensitivity βmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Black hole sensitivities in Einstein-scalar-Gauss-Bonnet gravity

Julié,

Silva,

Berti

et al. 2022

Preprint

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Exploring the small mass limit of stationary black holes in theories with Gauss–Bonnet terms

Fernandes

Mulryne

Delgado

2022

Class. Quantum Grav.

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In this work we examine the small mass limit of black holes, with and without spin, in theories where a scalar field is non-minimally coupled to a Gauss-Bonnet term. First, we provide an analytical example for a theory where a static closed-form solution with a small mass limit is known, and later use analytical and numerical techniques to explore this limit in standard scalar-Gauss-Bonnet theories with dilatonic, linear and quadratic-exponential couplings. In most cases studied here, we find an inner singularity that overlaps with the event horizon of the static black hole as the small mass limit is reached. Moreover, since solutions in this limit possess a non-vanishing Hawking temperature, a naked singularity is expected to be reached through evaporation, raising questions concerning the consistency of these theories altogether. On the other hand, we provide for the first time in this context an example of a coupling where the small mass limit is never reached, thus preferred from the point of view of cosmic censorship. Finally, we consider black holes with spin and numerically investigate how this changes the picture, using these to place the tightest upper bounds to date on the coupling constant for the dilatonic and linear theories, with $\sqrt{\overline{\alpha}} < 1$ km.

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Testing disformal non-circular deformation of Kerr black holes with LISA

Babichev,

Charmousis,

Doneva

et al. 2024

J. Cosmol. Astropart. Phys.

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There is strong observational evidence that almost every large galaxy has a supermassive black hole at its center. It is of fundamental importance to know whether such black holes are described by the standard Kerr solution in General Relativity (GR) or by another black hole solution. An interesting alternative is the so-called disformal Kerr black holes which exist within the framework of degenerate higher-order scalar-tensor (DHOST) theories of gravity. The departure from the standard Kerr black hole spacetime is parametrized by a parameter D, called disformal parameter. In the present work, we discuss the capability of LISA to detect the disformal parameter. For this purpose, we study Extreme Mass Ratio Inspirals (EMRI's) around disformal Kerr black holes within the framework of the quadrupole hybrid formalism. Even when the disformal parameter is very small, its effect on the globally accumulated phase of the gravitational waveform of an EMRI can be significant due to the large number of cycles in the LISA band made by the small compact object. We show that LISA will in principle be able to detect and measure extremely small values of the disformal parameter which in turn, can be seen as an assessment of LISA's ability to detect very small deviations from the Kerr geometry.

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Constraints on Einstein-dilation-Gauss-Bonnet gravity from Black Hole-Neutron Star Gravitational Wave Events

Cited by 5 publications

References 71 publications

Black hole sensitivities in Einstein-scalar-Gauss-Bonnet gravity

Black hole sensitivities in Einstein-scalar-Gauss-Bonnet gravity

Exploring the small mass limit of stationary black holes in theories with Gauss–Bonnet terms

Testing disformal non-circular deformation of Kerr black holes with LISA

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