Highly eccentric inspirals into a black hole

Osburn, Thomas; Warburton, Niels; Evans, Charles R.

doi:10.1103/physrevd.93.064024

Cited by 67 publications

(100 citation statements)

References 95 publications

(161 reference statements)

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“…These results further support the importance of deriving second-order self-force effects [101][102][103][104][105][106][107]. Previous studies have strongly relied on selfforce calculations for waveform modeling, source detection and parameter estimation studies, and have exhibited their applicability for extreme-and comparable-mass-ratio systems [59,99,[108][109][110][111][112][113][114][115][116][117]. Moving forward, it is necessary to develop new waveform models that enable the description of compact binaries whose components have nonzero spin and which evolve on eccentric orbits.…”

Section: Discussionsupporting

confidence: 69%

“…[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%

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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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Section: Discussionsupporting

confidence: 69%

Section: Introductionmentioning

confidence: 99%

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

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“…The results, corroborated by the use of several gauges and numerical techniques (see, e.g., Ref. [10] and references therein), have been already used to evolve extreme-mass-ratio-inspirals (EMRIs) around a Schwarzschild black-hole [60,61] and they represent a key input for EMRI waveform modeling schemes recently developed [62] and under development [63].…”

Section: Introductionmentioning

confidence: 65%

Quasicircular inspirals and plunges from nonspinning effective-one-body Hamiltonians with gravitational self-force information

et al. 2020

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The self-force program aims at accurately modeling relativistic two-body systems with a small mass ratio (SMR). In the context of the effective-one-body (EOB) framework, current results from this program can be used to determine the effective metric components at linear order in the mass ratio, resumming post-Newtonian (PN) dynamics around the test-particle limit in the process. It was shown in [Akcay et al., Phys. Rev. D 86 (2012)] that, in the original (standard) EOB gauge, the SMR contribution to the metric component g eff tt exhibits a coordinate singularity at the light-ring (LR) radius. In this paper, we adopt a different gauge for the EOB dynamics and obtain a Hamiltonian that is free of poles at the LR, with complete circular-orbit information at linear order in the mass ratio and non-circular-orbit and higher-order-in-mass-ratio terms up to 3PN order. We confirm the absence of the LR-divergence in such an EOB Hamiltonian via plunging trajectories through the LR radius. Moreover, we compare the binding energies and inspiral waveforms of EOB models with SMR, PN and mixed SMR-3PN information on a quasi-circular inspiral against numerical-relativity predictions. We find good agreement between NR simulations and EOB models with SMR-3PN information for both equal and unequal mass ratios. In particular, when compared to EOB inspiral waveforms with only 3PN information, EOB Hamiltonians with SMR-3PN information improves the modeling of binary systems with small mass ratios q 1/3, with a dephasing accumulated in ∼30 gravitational-wave (GW) cycles being of the order of few hundredths of a radian up to 4 GW cycles before merger.

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“…To date, all gravitational self-force calculations have been made by fixing the particle's motion to a geodesic of the background spacetime [52][53][54][55][56][57][58]. Inspirals are then computed by solving the equations of motion and making the approximation that the self-force at each instance is that of a particle moving along a tangent to the inspiraling worldline [59][60][61]. Quantifying the phase error induced by making this 'geodesic self-force approximation' requires comparison with a self-consistent inspiral where the self-force at each instance is the true self-force calculated as an integral over the past, inspiraling worldline.…”

Section: Introductionmentioning

confidence: 99%

Accelerated motion and the self-force in Schwarzschild spacetime

Heffernan

Ottewill

Warburton

et al. 2018

Class. Quantum Grav.

Self Cite

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We provide expansions of the Detweiler-Whiting singular field for a particle with a scalar field moving along arbitrary, planar accelerated trajectories in Schwarzschild spacetime. We transcribe these results into mode-sum regularization parameters, computing previously unknown terms that increase the convergence rate of the mode-sum. We test our results by computing the self-force along a variety of accelerated trajectories. For non-uniformly accelerated circular orbits we present results from a new 1+1D discontinuous Galerkin time-domain code which employs an effectivesource. We also present results for uniformly accelerated circular orbits and accelerated bound eccentric orbits computed within a frequency-domain treatment. Our regularization results will be useful for computing self-consistent self-force inspirals where the particle's worldline is accelerated with respect to the background spacetime.

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Highly eccentric inspirals into a black hole

Cited by 67 publications

References 95 publications

Complete waveform model for compact binaries on eccentric orbits

Complete waveform model for compact binaries on eccentric orbits

Quasicircular inspirals and plunges from nonspinning effective-one-body Hamiltonians with gravitational self-force information

Accelerated motion and the self-force in Schwarzschild spacetime

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