Eccentric black hole mergers and zoom-whirl behavior from elliptic inspirals to hyperbolic encounters

Gold, Roman; Brügmann, Bernd

doi:10.1103/physrevd.88.064051

Cited by 53 publications

(40 citation statements)

References 129 publications

(154 reference statements)

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“…Zooms and whirls have even been observed for hyperbolic orbits. Gold and Brügman showed orbits that exhibited a single whirl followed by a zoom to infinity [23]. Our focus will be on highly eccentric encounters similar to these, with the black holes reaching large separations quickly after a close encounter.…”

Section: Introductionmentioning

confidence: 97%

“…Other studies of zoom-whirl behavior in equal-mass, nonspinning binaries have been performed (see, e.g., [20,21]. These trajectories have also been studied for comparablemass Kerr black holes [10] and large-mass-ratio Kerr black holes [22], as well as for binary systems that contain one spinning black hole and one non-spinning black hole [11].…”

Section: Introductionmentioning

confidence: 99%

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Induced spins from scattering experiments of initially nonspinning black holes

et al. 2019

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When two relativistically boosted, nonspinning black holes pass by one another on a scattering trajectory, we might expect the tidal interaction to spin up each black hole. We present the first exploration of this effect, appearing at fourth post-Newtonian order, with full numerical relativity calculations. The basic set up for the calculations involves two free parameters: the initial boost of each black hole and the initial angle between their velocity vectors, with zero angle corresponding to a head-on trajectory. To minimize gauge effects, we measure final spins only if the black holes reach a final separation of at least 20M . Fixing the initial boost, we find that as the initial angle decreases toward the scattering/non-scattering limit, the spin-up grows nonlinearly. In addition, as initial boosts are increased from 0.42c to 0.78c, the largest observed final dimensionless spin on each black hole increases nonlinearly from 0.02 to 0.20. Based on these results, we conclude that much higher spin-ups may be possible with larger boosts, although achieving this will require improved numerical techniques.

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Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Induced spins from scattering experiments of initially nonspinning black holes

et al. 2019

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“…[44] at small eccentricity [34]; (vi) hybrid waveforms that describe highly eccentric systems: these waveforms describe the inspiral evolution using geodesic equations of motion, and the merger phase is modeled using a semianalytical prescription that captures the features of NR simulations [51]; (vii) self-force calculations for nonspinning BHs along eccentric orbits [52][53][54][55][56][57][58][59]; and (viii) NR simulations that explore the dynamics of eccentric binary systems [47,[60][61][62][63][64][65][66][67][68][69].…”

Section: Introductionmentioning

confidence: 99%

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

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We present a time domain waveform model that describes the inspiral, merger and ringdown of compact binary systems whose components are nonspinning, and which evolve on orbits with low to moderate eccentricity. The inspiral evolution is described using third-order post-Newtonian equations both for the equations of motion of the binary, and its far-zone radiation field. This latter component also includes instantaneous, tails and tails-of-tails contributions, and a contribution due to nonlinear memory. This framework reduces to the post-Newtonian approximant TaylorT4 at third postNewtonian order in the zero-eccentricity limit. To improve phase accuracy, we also incorporate higher-order post-Newtonian corrections for the energy flux of quasicircular binaries and gravitational self-force corrections to the binding energy of compact binaries. This enhanced prescription for the inspiral evolution is combined with a fully analytical prescription for the merger-ringdown evolution constructed using a catalog of numerical relativity simulations. We show that this inspiral-mergerringdown waveform model reproduces the effective-one-body model of Ref. [Y. Pan et al., Phys. Rev. D 89, 061501 (2014).] for quasicircular black hole binaries with mass ratios between 1 to 15 in the zero-eccentricity limit over a wide range of the parameter space under consideration. Using a set of eccentric numerical relativity simulations, not used during calibration, we show that our new eccentric model reproduces the true features of eccentric compact binary coalescence throughout merger. We use this model to show that the gravitational-wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasicircular, spin-aligned waveforms if the eccentricity e 0 of these systems when they enter the aLIGO band at a gravitational-wave frequency of 14 Hz satisfies e GW150914 0 ≤ 0.15 and e GW151226 0 ≤ 0.1. We also find that varying the spin combinations of the quasicircular, spin-aligned template waveforms does not improve the recovery of nonspinning, eccentric signals when e 0 ≥ 0.1. This suggests that these two signal manifolds are predominantly orthogonal.

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“…293 More recently, however, such collisions have received a fair amount of attention. 87,269,270,[294][295][296][297][298][299][300] Unfortunately, their rates are at least as difficult to estimate as those of GW-driven mergers. Collisions differ from gravitational wave-driven mergers in a number of ways.…”

Section: Gravitational Wave-driven Binary Mergers Vs Dynamic Collisionsmentioning

confidence: 99%

The multi-messenger picture of compact binary mergers

Rosswog

2015

Int. J. Mod. Phys. D

161

139

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In the last decade, enormous progress has been achieved in the understanding of the various facets of coalescing double neutron star and neutron black hole binary systems. One hopes that the mergers of such compact binaries can be routinely detected with the advanced versions of the ground-based gravitational wave detector facilities, maybe as early as in 2016. From the theoretical side, there has also been mounting evidence that compact binary mergers could be major sources of heavy elements and these ideas have gained recent observational support from the detection of an event that has been interpreted as a "macronova", an electromagnetic transient powered by freshly produced, radioactively decaying heavy elements. In addition, compact binaries are the most plausible triggers of short gamma-ray bursts (sGRBs) and the last decade has witnessed the first detection of a sGRB afterglow and subsequent observations have delivered a wealth of information on the environments in which such bursts occur. To date, compact binary mergers can naturally explain most -though not all-of the observed sGRB properties. This article reviews major recent developments in various areas related to compact binary mergers.

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Eccentric black hole mergers and zoom-whirl behavior from elliptic inspirals to hyperbolic encounters

Cited by 53 publications

References 129 publications

Induced spins from scattering experiments of initially nonspinning black holes

Induced spins from scattering experiments of initially nonspinning black holes

Complete waveform model for compact binaries on eccentric orbits

The multi-messenger picture of compact binary mergers

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