Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

Mroué, Abdul; Pfeiffer, Harald P.; Kidder, Lawrence E.; Teukolsky, Saul A.

doi:10.1103/physrevd.82.124016

Cited by 64 publications

(90 citation statements)

References 56 publications

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“…In this work we are not intent to touch this subtle problem involved in numerical relativity [74,75]. Instead, we take the similar recipe adopted in the above subsection to do the comparison.…”

Section: Comparison To Numerical Relativity Resultsmentioning

confidence: 99%

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Cao¹,

Han²

2017

Phys. Rev. D

144

134

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Binary black hole systems are among the most important sources for gravitational wave detection. And also they are good objects for theoretical research for general relativity. Gravitational waveform template is important to data analysis. Effective-one-body-numerical-relativity (EOBNR) model has played an essential role in the LIGO data analysis. For future space-based gravitational wave detection, many binary systems will admit somewhat orbit eccentricity. At the same time the eccentric binary is also an interesting topic for theoretical study in general relativity. In this paper we construct the first eccentric binary waveform model based on effective-one-body-numerical-relativity framework. Our basic assumption in the model construction is that the involved eccentricity is small. We have compared our eccentric EOBNR model to the circular one used in LIGO data analysis. We have also tested our eccentric EOBNR model against to another recently proposed eccentric binary waveform model; against to numerical relativity simulation results; and against to perturbation approximation results for extreme mass ratio binary systems. Compared to numerical relativity simulations with eccentricity as large as about 0.2, the overlap factor for our eccentric EOBNR model is better than 0.98 for all tested cases including spinless binary and spinning binary; equal mass binary and unequal mass binary. Hopefully our eccentric model can be the start point to develop a faithful template for future space-based gravitational wave detectors.

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Section: Comparison To Numerical Relativity Resultsmentioning

confidence: 99%

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Cao¹,

Han²

2017

Phys. Rev. D

144

134

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show abstract

“…Periastron advance can be studied in aligned spin binaries and generic binaries [54,65,66], using simulations with different eccentricities. This allows the first calculation of the gravitational self-force contribution to the periastron advance for spinning binaries [67].…”

Section: Discussionmentioning

confidence: 99%

“…The catalog includes (i) 62 new single-spin simulations with χ A = 0.5, χ B = 0 ranging from q = 1 to q = 8, which extend efforts by the NINJA-2 collaboration [19] (which contains only three unequal mass, aligned spin simulations and no precessing simulations) and the NRAR collaboration [20] (which contains spinning simulations only for q ≤ 3); (ii) 32 new simulations with random mass ratios q ∈ [1, 2] and random spins (χ A , χ B ≤ 0.5); (iii) 16 q = 1 simulations with equal, aligned spins [23,52,53], including one new simulation with the highest BH spin to date (χ A = χ B = 0.98); (iv) a high mass ratio, high-spin (q = 6, χ A = 0.9, χ B = 0.3), precessing simulation intended to test numerical capabilities; (v) 32 non-spinning simulations, including mass ratios q = 1.5, 5, 8, not considered in [22]. Also included are new simulations of different orbital eccentricities and durations, which facilitate calculation of periastron advance [54] and efficient initial data generation [34].…”

Section: Techniquesmentioning

confidence: 99%

Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy

et al. 2013

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This paper presents a publicly available catalog of 174 numerical binary black-hole simulations following up to 35 orbits. The catalog includes 91 precessing binaries, mass ratios up to 8:1, orbital eccentricities from a few percent to 10 −5 , black-hole spins up to 98% of the theoretical maximum, and radiated energies up to 11.1% of the initial mass. We establish remarkably good agreement with post-Newtonian precession of orbital and spin directions for two new precessing simulations, and we discuss other applications of this catalog. Formidable challenges remain: e.g., precession complicates the connection of numerical and approximate analytical waveforms, and vast regions of the parameter space remain unexplored.

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“…Furthermore, as shown in e.g. [83], it is difficult to determine K for simulations with almost vanishing eccentricity. For these reasons we focus on the MS1b-150100 setup which has the lowest starting frequency.…”

Section: Eob-nr Comparisonmentioning

confidence: 99%

“…From the eccentricity indicator we calculate the PA following the work of [83]. We determine the times t k of the extrema of e corresponding to perihelia and aphelia and compute the orbital phase φ Ω and GW phase φ 22 at these times t k .…”

Section: B Extracting the Periastron Advance From Nr Simulationsmentioning

confidence: 99%

Comprehensive comparison of numerical relativity and effective-one-body results to inform improvements in waveform models for binary neutron star systems

Dietrich

Hinderer

2017

Phys. Rev. D

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We present a detailed comparison between tidal effective-one-body (EOB) models and new stateof-the-art numerical relativity simulations for non-spinning binary neutron star systems. This comparison is the most extensive one to date, covering a wide range in the parameter space and encompassing the energetics of the binary, the periastron advance, the time and frequency evolution of the gravitational wave phase for the dominant mode, and several subdominant modes. We consider different EOB models with tidal effects that have been proposed, including the model with dynamical tides of [Phys.Rev.Lett. 116 (2016) no.18, 181101] and the gravitational self-force (GSF) inspired tidal EOB model of [Phys.Rev.Lett. 114 (2015) no.16, 161103]. The EOB model with dynamical tides leads to the best representation of the systems considered here, however, the differences to the GSF-inspired model are small. A common feature is that for systems where matter effects are large, i.e. stiff equations of state or small total masses, all EOB models underestimate the tidal effects and differences to the results from numerical relativity simulations become noticeable near the merger. We analyze this regime to diagnose the shortcomings of the models in the late inspiral, where the two neutron stars are no longer isolated bodies moving in vacuum. Our work will serve to guide further advances in modeling these systems.

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Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

Cited by 64 publications

References 56 publications

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy

Comprehensive comparison of numerical relativity and effective-one-body results to inform improvements in waveform models for binary neutron star systems

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