Gravitational Radiation and the Motion of Two Point Masses

Peters, P. C.

doi:10.1103/physrev.136.b1224

Cited by 2,261 publications

(2,526 citation statements)

References 5 publications

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“…This explains why the thin and thick lines corresponding to the initial and final histograms coincide for q < 0.1. The gravitationalwave inspiral time is inversely proportional to the binary's symmetric mass ratio η = q/(1 + q) 2 [60], making it hard to preserve accuracy over long PN time evolutions for q < 0.1. However, Schnittman [20] showed that spinorbit resonances only become important inside a "resonance locking" radius r lock /M ≈ [(1 + q 2 )/(1 − q 2 )] 2 .…”

Section: Resultsmentioning

confidence: 99%

“…Although dynamical friction damped the orbital eccentricity at the large separations of the Dotti et al simulations [17], after the formation of a circumbinary disk the orbital eccentricity again grows to a limiting value e crit ≃ 0.7 [59]. Gravitational radiation circularizes the binary after it decouples from the circumbinary disk [60], but the binary could still have considerable residual eccentricity e LISA ∝ M −0.73 q −1.2 when the frequency of the fundamental GW harmonic reaches f LISA = 10 −4 Hz [59,61]. We will neglect residual eccentricity during the inspiral and any effects it might have on PN spin alignment.…”

Section: Spin Directionsmentioning

confidence: 99%

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Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

2012

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Recent numerical relativity simulations have shown that the final black hole produced in a binary merger can recoil with a velocity as large as 5, 000 km/s. Because of enhanced gravitational-wave emission in the so-called "hang-up" configurations, this maximum recoil occurs when the black-hole spins are partially aligned with the orbital angular momentum. We revisit our previous statistical analysis of post-Newtonian evolutions of black-hole binaries in the light of these new findings. We demonstrate that despite these new configurations with enhanced recoil velocities, spin alignment during the post-Newtonian stage of the inspiral will still significantly suppress (or enhance) kick magnitudes when the initial spin of the more massive black hole is more (or less) closely aligned with the orbital angular momentum than that of the smaller hole. We present a preliminary study of how this post-Newtonian spin alignment affects the ejection probabilities of supermassive black holes from their host galaxies with astrophysically motivated mass ratio and initial spin distributions. We find that spin alignment suppresses (enhances) ejection probabilities by ∼ 40% (20%) for an observationally motivated mass-dependent galactic escape velocity, and by an even greater amount for a constant escape velocity of 1,000 km/s. Kick suppression is thus at least a factor two more efficient than enhancement.

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Section: Resultsmentioning

confidence: 99%

Section: Spin Directionsmentioning

confidence: 99%

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

2012

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“…Radiation reaction reduces eccentricity during the inspiral of a binary compact object, as shown by the postNewtonian calculation by Peters [16]. Using the quadrupole approximation, Peters derived the evolution of the orbital eccentricity during the inspiral caused by the emission of gravitational waves.…”

Section: Behavior Of Eccentricity During Inspiralmentioning

confidence: 99%

“…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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“…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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Gravitational Radiation and the Motion of Two Point Masses

Cited by 2,261 publications

References 5 publications

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

Measuring orbital eccentricity and periastron advance in quasicircular black hole simulations

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

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