Erratum: Neutron stars in Einstein-Aether theory [Phys. Rev. D<b>76</b>, 042003 (2007)]

Eling, Christopher; Jacobson, Ted; Miller, M. Coleman

doi:10.1103/physrevd.80.129906

Cited by 38 publications

(50 citation statements)

References 41 publications

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“…Of course, such a method to test modified gravity theories is not new; it has been considered in e.g. [68] for Einstein-Aether theory and [69] for EinsteinDilaton-Gauss-Bonnet theory. The horizontal dashed line in Fig.…”

Section: A Massive Millisecond Pulsar J1614-2230mentioning

confidence: 99%

Isolated and binary neutron stars in dynamical Chern-Simons gravity

et al. 2013

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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: A Massive Millisecond Pulsar J1614-2230mentioning

confidence: 99%

Isolated and binary neutron stars in dynamical Chern-Simons gravity

et al. 2013

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“…The solution inside a fluid star has been found by numerical integration, both for constant density 18 and for realistic neutron star equations of state. 20 The maximum masses for neutron stars range from about 6 to 15% smaller than in GR when c 14 = 1, depending on the equation of state. The corresponding surface redshifts can be as much as 10% larger than in GR for the same mass.…”

Section: Spherically Symmetric Stars and Black Holesmentioning

confidence: 99%

Einstein-Æther Gravity: Theory and Observational Constraints

Jacobson¹

2008

CPT and Lorentz Symmetry

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“…It is also important to investigate neutron stars or black holes. In Einstein-Aether theory, these features are investigated and show interesting differences from the case in general relativity [18,19,20]. As for TeVeS, black holes have been investigated only for the cases where the scalar field diverges at the horizon [8,13] or the scalar field is constant [16].…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Post-Newtonian parameters in the tensor-vector-scalar theory

Tamaki

2008

Phys. Rev. D

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We investigate post-Newtonian parameters in the tensor-vector-scalar (TeVeS) theory in a general setting while previous researches have been restricted to spherically symmetric cases. Based on the assumption that both the physical and Einstein metrics have Minkowski metric at the zeroth order, we show γ = 1 as in the previous researches. We find two remarkable things for other parameters. The first is the value β = 1 while it has been reported that β = 1 for the case when the vector field is not purely timelike. This discrepancy occurs from the above assumption which is natural as a starting point. The second is the result that the Newtonian potential must be static to be consistent with the vector equation. As a result, we cannot determine α1 and α2. We consider that it is related to the instability against linear perturbation and occurrence of caustic singularities for various initial perturbations which have been reported recently.

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Erratum: Neutron stars in Einstein-Aether theory [Phys. Rev. D76, 042003 (2007)]

Cited by 38 publications

References 41 publications

Isolated and binary neutron stars in dynamical Chern-Simons gravity

Isolated and binary neutron stars in dynamical Chern-Simons gravity

Einstein-Æther Gravity: Theory and Observational Constraints

Post-Newtonian parameters in the tensor-vector-scalar theory

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