Erratum: Effective-one-body Hamiltonian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins [Phys. Rev. D<b>87</b>, 124036 (2013)]

Balmelli, Simone; Jetzer, Philippe

doi:10.1103/physrevd.90.089905

Cited by 13 publications

(34 citation statements)

References 41 publications

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“…[17], which is robust enough for BNS realistic spin values (dimensionless magnitude χ A,B 0.1). The spin-orbit interaction is taken at NNLO [23], the spin-spin at leading-order [24]. The spin gauge freedom is fixed according to [23,25].…”

Section: Is Analytically Known At 4pn Accuracy and Formally Readsmentioning

confidence: 99%

Quasiuniversal Properties of Neutron Star Mergers

Bernuzzi¹,

et al. 2014

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Binary neutron star mergers are studied using nonlinear 3+1 numerical relativity simulations and the analytical effective-one-body (EOB) model. The EOB model predicts quasiuniversal relations between the mass-rescaled gravitational wave frequency and the binding energy at the moment of merger, and certain dimensionless binary tidal coupling constants depending on the stars Love numbers, compactnesses and the binary mass ratio. These relations are quasiuniversal in the sense that, for a given value of the tidal coupling constant, they depend significantly neither on the equation of state nor on the mass ratio, though they do depend on stars spins. The spin dependence is approximately linear for small spins aligned with the orbital angular momentum. The quasiuniversality is a property of the conservative dynamics; nontrivial relations emerge as the binary interaction becomes tidally dominated. This analytical prediction is qualitatively consistent with new, multi-orbit numerical relativity results for the relevant case of equal-mass irrotational binaries. Universal relations are thus expected to characterize neutron star mergers dynamics. In the context of gravitational wave astronomy, these universal relations may be used to constrain the neutron star equation of state using waveforms that model the merger accurately.

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Section: Is Analytically Known At 4pn Accuracy and Formally Readsmentioning

confidence: 99%

Quasiuniversal Properties of Neutron Star Mergers

Bernuzzi¹,

et al. 2014

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“…The EOB conservative dynamics and waveforms have been extended to spinning BHs in [271,[286][287][288][289][290][291] and [292], respectively. In particular, motivated by the construction of a EOB Hamiltonian for spinning systems, that reduces to the Hamiltonian of a spinning particle in the extreme-mass ratio limit, [287] worked out, for the first time, the Hamiltonian of a spinning particle in curved spacetime at all orders in PN theory and linear in the particle's spin.…”

Section: The Effective-one-body Formalismmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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“…[28], but presents some basic structural differences with respect to Refs. [18,21,28,30]. The most important ones are the introduction of a new variable (the centrifugal radius r c ), which plays a central role for the description of quadratic spin effects, and a simplification of the spin-orbit structure.…”

Section: Introductionmentioning

confidence: 95%

“…More recently, an EOB Hamiltonian reproducing the correct NLO spin-spin coupling has been proposed [28][29][30], where the terms in question are included by a subleading-order modification of various squared-spin terms. An unpleasant feature of this approach is that the so-obtained effective squared-spin acquires a momentum dependence that cannot be removed by any gauge tuning, and that greatly complicates the analytic form of the Hamiltonian.…”

Section: Introductionmentioning

confidence: 99%

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New effective-one-body Hamiltonian with next-to-leading order spin-spin coupling

Balmelli

Damour

2015

Phys. Rev. D

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We present a new effective-one-body (EOB) Hamiltonian with next-to-leading order (NLO) spinspin coupling for black hole binaries endowed with arbitrarily oriented spins. The Hamiltonian is based on the model for parallel spins and equatorial orbits developed in [Physical Review D 90, 044018 (2014)], but differs from it in several ways. In particular, the NLO spin-spin coupling is not incorporated by a redefinition of the centrifugal radius rc, but by separately modifying certain sectors of the Hamiltonian, which are identified according to their dependence on the momentum vector. The gauge-fixing procedure we follow allows us to reduce the 25 different terms of the NLO spin-spin Hamiltonian in Arnowitt-Deser-Misner coordinates to only 9 EOB terms. This is an improvement with respect to the EOB model recently proposed in [Physical Review D 91, 064011 (2015)], where 12 EOB terms were involved. Another important advantage is the remarkably simple momentum structure of the spin-spin terms in the effective Hamiltonian, which is simply quadratic up to an overall square root. Moreover, a Damour-Jaranowski-Schäfer-type gauge could be established, thus allowing one to concentrate, in the case of circular and equatorial orbits, the whole spin-spin interaction in a single radial potential.

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Erratum: Effective-one-body Hamiltonian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins [Phys. Rev. D87, 124036 (2013)]

Cited by 13 publications

References 41 publications

Quasiuniversal Properties of Neutron Star Mergers

Quasiuniversal Properties of Neutron Star Mergers

Sources of Gravitational Waves: Theory and Observations

New effective-one-body Hamiltonian with next-to-leading order spin-spin coupling

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