Gravitational Radiation from Point Masses in a Keplerian Orbit

Peters, P. C.; Mathews, Jon

doi:10.1103/physrev.131.435

Cited by 1,427 publications

(1,589 citation statements)

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“…This is very likely a good approximation for binaries formed in fields as radiation back reaction circularises a binary much faster than the orbit decays [399,400]. However, eccentric binaries may form through Kozai mechanism or dynamical capture in dense stellar environments [401][402][403][404] and in this case the eccentricity can be large at merger.…”

Section: Challengesmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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Section: Challengesmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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“…Given that the gravitational radiation causes the orbits of isolated binary systems to circularize [52,53], we will consider only the PN-inspirals in quasicircular orbits with masses m i (i = 1, 2) and (the magnitude of) spins S i that are (anti-)aligned and normal to the orbital plane, but they have an arbitrary mass ratio. (All throughout, we use geometric units, where G = c = 1, with the useful conversion factor 1M ⊙ = 1.477 km = 4.926 × 10 −6 s.) In this adiabatic setup, the GW phase of the dominant harmonic is twice the orbital phase [20].…”

Section: Goals and Motivationsmentioning

confidence: 99%

Post-Newtonian templates for binary black-hole inspirals: the effect of the horizon fluxes and the secular change in the black-hole masses and spins

Isoyama¹,

Nakano²

2017

Class. Quantum Grav.

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Abstract. Black holes (BHs) in an inspiraling compact binary system absorb the gravitational-wave (GW) energy and angular-momentum fluxes across their event horizons and this leads to the secular change in their masses and spins during the inspiral phase. The goal of this paper is to present ready-to-use, 3.5 postNewtonian (PN) template families for spinning, non-precessing, binary BH inspirals in quasicircular orbits, including the 2.5PN and 3.5PN horizon-flux contributions as well as the correction due to the secular change in the BH masses and spins through 3.5PN order, respectively, in phase. We show that, for binary BHs observable by Advanced LIGO with high mass ratios (larger than ∼ 10) and large aligned-spins (larger than ∼ 0.7), the mismatch between the frequency-domain template with and without the horizon-flux contribution is typically above the 3% mark. For (supermassive) binary BHs observed by LISA, even a moderate mass-ratios and spins can produce a similar level of the mismatch. Meanwhile, the mismatch due to the secular time variations of the BH masses and spins is well below the 1% mark in both cases, hence this is truly negligible. We also point out that neglecting the cubic-in-spin, point-particle phase term at 3.5PN order would deteriorate the effect of BH absorption in the template.

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“…During the inspiral of an isolated binary, the orbit circularizes via the emission of gravitational waves [16,17]. As a result, even binaries starting with some eccentricity at the beginning of their stellar evolution are expected to have negligible eccentricity by the time the frequency of the emitted gravitational radiation enters the frequency band of ground based detectors.…”

Section: Introductionmentioning

confidence: 99%

Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

et al. 2010

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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-Newtonian results. Finally, we measure the periastron advance of nonspinning binary black holes, and we compare them to post-Newtonian approximations. With the low uncertainty in the measurement of the periastron advance, we positively detect deviations between fully numerical simulations and post-Newtonian calculations.

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Gravitational Radiation from Point Masses in a Keplerian Orbit

Cited by 1,427 publications

References 1 publication

Sources of Gravitational Waves: Theory and Observations

Sources of Gravitational Waves: Theory and Observations

Post-Newtonian templates for binary black-hole inspirals: the effect of the horizon fluxes and the secular change in the black-hole masses and spins

Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

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