2010
DOI: 10.1103/physrevd.82.124016
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Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

Abstract: We compare different methods of computing the orbital eccentricity of quasicircular binary black-hole systems using the orbital variables and gravitational-wave phase and frequency. For eccentricities of about a per cent, most methods work satisfactorily. For small eccentricity, however, the gravitational-wave phase allows a particularly clean and reliable measurement of the eccentricity. Furthermore, we measure the decay of the orbital eccentricity during the inspiral and find reasonable agreement with post-N… Show more

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Cited by 67 publications
(91 citation statements)
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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%
“…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%
“…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%
“…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%