Amplification of superkicks in black-hole binaries through orbital eccentricity

Sperhake, Ulrich; Rosca-Mead, Roxana; Gerosa, Davide; Berti, Emanuele

doi:10.1103/physrevd.101.024044

Cited by 16 publications

(22 citation statements)

References 87 publications

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“…Refs. [67,68]). Figure 10 shows the cross-validation errors of NRSur2dq1EccRemnant in predicting the remnant mass and spin.…”

Section: Nrsur2dq1eccremnant Errorsmentioning

confidence: 99%

“…Apart from the waveform prediction, BBH remnant modeling from eccentric sources is also of crucial astrophysical importance [65][66][67][68]. For example, recoils from eccentric mergers can be up to 25% higher than the circular case [67,68], which results in a higher likelihood of ejections from astrophysical hosts like star clusters and galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

et al. 2021

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We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors. We introduce a new surrogate waveform model, NRSur2dq1Ecc, using 47 nonspinning, equalmass waveforms with eccentricities up to 0.2 when measured at a reference time of 5500M before merger. This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger. The model includes the (2,2), (3,2), and (4,4) spin-weighted spherical harmonic modes. We also build a final black hole model, NRSur2dq1Ec-cRemnant, which models the mass, and spin of the remnant black hole. We show that our waveform model can accurately predict numerical relativity waveforms with mismatches ≈10 −3 , while the remnant model can recover the final mass and dimensionless spin with absolute errors smaller than ≈5 × 10 −4 M and ≈2 × 10 −3 respectively. We demonstrate that the waveform model can also recover subtle effects like mode mixing in the ringdown signal without any special ad hoc modeling steps. Finally, we show that despite being trained only on equal-mass binaries, NRSur2dq1Ecc can be reasonably extended up to mass ratio q ≈ 3 with mismatches ≃10 −2 for eccentricities smaller than ∼0.05 as measured at a reference time of 2000M before merger. The methods developed here should prove useful in the building of future eccentric surrogate models over larger regions of the parameter space.

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“…Refs. [67,68]). Figure 10 shows the cross-validation errors of NRSur2dq1EccRemnant in predicting the remnant mass and spin.…”

Section: Nrsur2dq1eccremnant Errorsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

et al. 2021

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“…We mostly focus on the eccentricity parameter e t in harmonic coordinates, 2 as in Ref. [42]. This estimate should be taken with a pinch of salt due to the relatively small initial binary separations D in our simulations.…”

Section: B Black-hole Binary Configurationsmentioning

confidence: 99%

“…Early calculations in the close-limit approximation [18] predicted a kick proportional to 1 þ e for small eccentricities, e ≲ 0.1. More recently, numerical relativity calculations led to the conclusion that eccentricity can lead to an approximate 25% increase in recoil velocities for superkick configurations with moderate eccentricities [42].…”

Section: Introductionmentioning

confidence: 99%

Anomalies in the gravitational recoil of eccentric black-hole mergers with unequal mass ratios

et al. 2021

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The radiation of linear momentum imparts a recoil (or "kick") to the center of mass of a merging blackhole binary system. Recent numerical relativity calculations have shown that eccentricity can lead to an approximate 25% increase in recoil velocities for equal-mass, spinning binaries with spins lying in the orbital plane ("superkick" configurations) [U. Sperhake et al. Phys. Rev. D 101, 024044 (2020)]. Here we investigate the impact of nonzero eccentricity on the kick magnitude and gravitational-wave emission of nonspinning, unequal-mass black hole binaries. We confirm that nonzero eccentricities at merger can lead to kicks which are larger by up to ∼25% relative to the quasicircular case. We also find that the kick velocity v has an oscillatory dependence on eccentricity, which we interpret as a consequence of changes in the angle between the infall direction at merger and the apoapsis (or periapsis) direction.

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“…For these systems, the spins interact with the orbital angular momentum as well as with each other, causing the orbital plane to precess [24]. The kick velocity of these systems can reach up to 5000 km/s for certain fine-tuned configurations [25][26][27][28][29][30], earning them the moniker of "superkicks". Such velocities are larger than the escape velocity of even the most massive galaxies.…”

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Extracting the Gravitational Recoil from Black Hole Merger Signals

2020

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Gravitational waves carry energy, angular momentum, and linear momentum. In generic binary black hole mergers, the loss of linear momentum imparts a recoil velocity, or a "kick", to the remnant black hole. We exploit recent advances in gravitational waveform and remnant black hole modeling to extract information about the kick from the gravitational wave signal. Kick measurements such as these are astrophysically valuable, enabling independent constraints on the rate of second-generation mergers. Further, we show that kicks must be factored into future ringdown tests of general relativity with third-generation gravitational wave detectors to avoid systematic biases. We find that, although little information can be gained about the kick for existing gravitational wave events, interesting measurements will soon become possible as detectors improve. We show that, once LIGO and Virgo reach their design sensitivities, we will reliably extract the kick velocity for generically precessing binaries-including the so-called superkicks, reaching up to 5000 km/s.

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Amplification of superkicks in black-hole binaries through orbital eccentricity

Cited by 16 publications

References 87 publications

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: Comparable mass, nonspinning case

Anomalies in the gravitational recoil of eccentric black-hole mergers with unequal mass ratios

Extracting the Gravitational Recoil from Black Hole Merger Signals

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