Erratum: Slowly rotating black holes in dynamical Chern-Simons gravity: Deformation quadratic in the spin [Phys. Rev. D 86, 044037 (2012)]

Yagi, Kent; Yunes, Nicolás; Tanaka, Takahiro

doi:10.1103/physrevd.89.049902

Cited by 117 publications

(169 citation statements)

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“…Currently, the only constraints on this theory come from Solar System observations [24], by comparing the CS correction to gravitomagnetic precession to observations with Gravity Probe B, and from table top [25] experiments, by requiring that no CS corrections are present above the smallest gravitational length scales sampled experimentally on Earth. These tests lead to comparable constraints, namely √ α < 10 8 km, where α is the dimensional CS coupling constant.…”

Section: Introductionmentioning

confidence: 99%

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Isolated and binary neutron stars in dynamical Chern-Simons gravity

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In Ref.[1], the Chern-Simons correction to the osculating orbital elements due to the dipole-dipole interaction for the scalar field was derived in Eq. (130) by integrating out the interaction Lagrangian, which was taken to be the kinetic term for the scalar field [Eq. (122) in [1]], using the scalar field solution. However, such kinetic term only leads to the left-hand side of the evolution equation for the scalar field, i.e.where J is the effective source term of the scalar field equation [2]. In order to obtain the correct interaction Lagrangian, one also needs to include the source term (L source ) that reproduces the right-hand side of the above evolution equation. The Lagrangian density for such an additional term is given by −ϑJ. Therefore, Eq. (126) needs to be changed towhere L source,int is the interaction part of the source term Lagrangian density. Notice that, by accounting for such additional term, the sign of the interaction Lagrangian now flips. This means that the sign in Eqs. (127), (129) and (130) needs to be reversed. The results in Sec. IX B are unaffected since we have neglected contribution from the dipole-dipole interaction because the spin of the secondary pulsar in the double binary pulsar is much smaller than that of the primary. We also report errors in App. B of [1]. In this appendix, we calculated dissipative corrections to the energy and angular momentum energy flux emitted from neutron star binaries based on calculations in [2]. However, some terms in the perturbed scalar and metric field equations were not properly accounted for in [2]. Taking these terms into account, we found that corrections to the gravitational energy and angular momentum flux due to metric perturbations enter at third post-Newtonian order relative to general relativity, which is of 1 post-Newtonian order higher than the effect due to the scalar field. Therefore, Apps. B.1.b and B.2.b in [1] are now irrelevant. We discuss this in more detail in [3].On the other hand, the scalar energy flux in App. B.1.a is affected as follows. First, the far-zone solution for the scalar field in Eq. (B3) becomesThen, the scalar energy flux in Eqs. (B5) and (B6) becomesrespectively. Finally, Eq. (B8) is corrected to T. Tanaka, Phys. Rev., D85, 064022 (2012), arXiv:1110.5950 [gr-qc].[3] K. Yagi, L. C. Stein, N. Yunes, and T. Tanaka, Phys. Rev., D93, 029902 (2016D93, 029902 ( ), arXiv:1110. We study isolated and binary neutron stars in dynamical Chern-Simons gravity. This theory modifies the Einstein-Hilbert action through the introduction of a dynamical scalar field coupled to the Pontryagin density. We here treat this theory as an effective model, working to leading order in the Chern-Simons coupling. We first construct isolated neutron star solutions in the slow-rotation expansion to quadratic order in spin. We find that isolated neutron stars acquire a scalar dipole charge that corrects its spin angular momentum to linear order in spin and corrects its mass and quadrupole moment to quadratic order in spin, as measured by ...

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Section: Introductionmentioning

confidence: 99%

“…Non-rotating BHs are described by the Schwarzschild metric, but rotating ones are not. Analytic slowly-rotating BH solutions have been constructed to linear order in spin [40,41] and to quadratic order in spin [25] within the small-coupling approximation, i.e. linearizing all expressions in the CS coupling.…”

Section: Introductionmentioning

confidence: 99%

Isolated and binary neutron stars in dynamical Chern-Simons gravity

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“…There are a wide class of theories that agree with GR in the slow motion, weak field regime, and pass all existing tests, yet differ significantly in the strong field, dynamical regime probed by binary inspiral and merger, e.g. dynamical Chern-Simons gravity [46][47][48][49][50][51][52][53][54][55]. We show that GWs from these types of theories could be missed entirely by searches using GR templates.…”

Section: Introductionmentioning

confidence: 98%

Mismodeling in gravitational-wave astronomy: The trouble with templates

2014

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Waveform templates are a powerful tool for extracting and characterizing gravitational wave signals, acting as highly restrictive priors on the signal morphologies that allow us to extract weak events buried deep in the instrumental noise. The templates map the waveform shapes to physical parameters, thus allowing us to produce posterior probability distributions for these parameters. However, there are attendant dangers in using highly restrictive signal priors. If strong field gravity is not accurately described by General Relativity (GR), then using GR templates may result in fundamental bias in the recovered parameters, or even worse, a complete failure to detect signals.Here we study such dangers, concentrating on three distinct possibilities. First, we show that there exist modified theories compatible with all existing observations that would fail to be detected by the LIGO/Virgo network using searches based on GR templates, but which would be detected using a one parameter post-Einsteinian extension. Second, we study modified theories that produce departures from GR that turn on suddenly at a critical frequency, producing waveforms that do not directly fit into the simplest parameterized post-Einsteinian (ppE) scheme. We show that even the simplest ppE templates are still capable of picking up these strange signals and diagnosing a departure from GR. Third, we study whether using inspiral-only ppE waveforms for signals that include merger and ringdown can lead to problems in misidentifying a GR departure. We present a simple technique that allows us to self-consistently identify the inspiral portion of the signal, and thus remove these potential biases, allowing GR tests to be performed on higher mass signals that merge within the detector band. We close by studying a parameterized waveform model that may allow us to test GR using the full inspiral-merger-ringdown signal.

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“…Moreover, the α-dependence is the stronger the smaller j. We did not go beyond α = 2, since the strongest current observational upper bound on α, obtained from low-mass X-ray binaries, is slightly less than this value (in the units employed) [12,36].…”

Section: Rotating Neutron Starsmentioning

confidence: 99%

Quadrupole moments of rapidly rotating compact objects in dilatonic Einstein-Gauss-Bonnet theory

2014

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We consider rapidly rotating black holes and neutron stars in dilatonic Einstein-Gauss-Bonnet (EGBd) theory and determine their quadrupole moments, which receive a contribution from the dilaton. The quadrupole moment of EGBd black holes can be considerably larger than the Kerr value. For neutron stars, the universality property of theÎ-Q relation between the scaled moment of inertia and the scaled quadrupole moment appears to extend to EGBd theory.

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Erratum: Slowly rotating black holes in dynamical Chern-Simons gravity: Deformation quadratic in the spin [Phys. Rev. D 86, 044037 (2012)]

Cited by 117 publications

References 3 publications

Isolated and binary neutron stars in dynamical Chern-Simons gravity

Isolated and binary neutron stars in dynamical Chern-Simons gravity

Mismodeling in gravitational-wave astronomy: The trouble with templates

Quadrupole moments of rapidly rotating compact objects in dilatonic Einstein-Gauss-Bonnet theory

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