Estimating effective higher order terms in the post-Newtonian binding energy and gravitational-wave flux: Nonspinning compact binary inspiral

Kapadia, S. J.; Johnson-McDaniel, Nathan K.; Ajith, P.

doi:10.1103/physrevd.93.024006

Cited by 3 publications

(4 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Furthermore, building upon Refs. [99,100], we will amend the energy flux prescription, _ Eðx; ηÞ 6PN , by constraining missing η 2 corrections in the energy flux expression used in Eq. (17).…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionmentioning

confidence: 99%

“…We will further improve the inspiral dynamics by including terms at second order in symmetric-mass ratio. Furthermore, building up on [99,100], we will amend the energy flux prescription, Ė(x, η) 6PN , by constraining missing η 2 corrections in the energy flux expression used in Eq. 17.…”

Section: Discussionmentioning

confidence: 99%

Complete waveform model for compact binaries on eccentric orbits

et al. 2017

View full text Add to dashboard Cite

show abstract

“…See also Ref [137]. for a recent attempt to address the issue of unknown PN corrections by fitting higher-order terms in the orbital energy and energy flux to EOBNR calculations.…”

mentioning

confidence: 99%

Gravitational-wave phasing for low-eccentricity inspiralling compact binaries to 3PN order

et al. 2016

View full text Add to dashboard Cite

Although gravitational radiation causes inspiralling compact binaries to circularize, a variety of astrophysical scenarios suggest that binaries might have small but nonnegligible orbital eccentricities when they enter the low-frequency bands of ground-and space-based gravitational-wave detectors. If not accounted for, even a small orbital eccentricity can cause a potentially significant systematic error in the mass parameters of an inspiralling binary [M. Favata, Phys. Rev. Lett. 112, 101101 (2014)]. Gravitational-wave search templates typically rely on the quasi-circular approximation, which provides relatively simple expressions for the gravitational-wave phase to 3.5 post-Newtonian (PN) order. Damour, Gopakumar, Iyer, and others have developed an elegant but complex quasiKeplerian formalism for describing the post-Newtonian corrections to the orbits and waveforms of inspiralling binaries with any eccentricity. Here we specialize the quasi-Keplerian formalism to binaries with low eccentricity. In this limit the non-periodic contribution to the gravitational-wave phasing can be expressed explicitly as simple functions of frequency or time, with little additional complexity beyond the well-known formulas for circular binaries. These eccentric phase corrections are computed to 3PN order and to leading order in the eccentricity for the standard PN approximants. For a variety of systems these eccentricity corrections cause significant corrections to the number of gravitational wave cycles that sweep through a detector's frequency band. This is evaluated using several measures, including a modification of the useful cycles. By comparing to numerical solutions valid for any eccentricity, we find that our analytic solutions are valid up to e0 0.1 for comparable mass systems, where e0 is the eccentricity when the source enters the detector band. We also evaluate the role of periodic terms that enter the phasing and discuss how they can be incorporated into some of the PN approximants. While the eccentric extension of the PN approximants is our main objective, this work collects a variety of results that may be of interest to others modeling eccentric relativistic binaries. This includes a consistent eccentricity expansion of the Newtonian-order polarizations and a comparison of quasi-Keplerian results with numerical simulations. In addition to applications in gravitational wave data analysis, the formulas derived here could be of use in comparing PN theory with numerical relativity or self-force calculations of eccentric binaries. They could also be useful in the construction of phenomenological inspiral-merger-ringdown waveforms that include eccentricity effects.

show abstract

“…While it is obvious that the fit can be used to directly test the dynamics inferred from waveform models, it might also be used to constrain higher order PN terms, see e.g. [68]. Additionally, an alternative calibration of the EOB Apotential is possible.…”

Section: B Comparison With Waveform Approximantsmentioning

confidence: 99%

Assessing the energetics of spinning binary black hole systems

et al. 2018

View full text Add to dashboard Cite

In this work we study the dynamics of spinning binary black hole systems in the strong field regime. For this purpose we extract from numerical relativity simulations the binding energy, specific orbital angular momentum, and gauge-invariant orbital frequency. The goal of our work is threefold: First, we extract the individual spin contributions to the binding energy, in particular the spin-orbit, spin-spin, and cubic-in-spin terms. Second, we compare our results with predictions from waveform models and find that while post-Newtonian approximants are not capable of representing the dynamics during the last few orbits before merger, there is good agreement between our data and effective-one-body approximants as well as the numerical relativity surrogate models. Finally, we present phenomenological representations for the binding energy for non-spinning systems with mass ratios up to q = 10 and for the spin-orbit interaction for mass ratios up to q = 8 obtaining accuracies of 0.1% and 6%, respectively.

show abstract

Estimating effective higher order terms in the post-Newtonian binding energy and gravitational-wave flux: Nonspinning compact binary inspiral

Cited by 3 publications

References 41 publications

Complete waveform model for compact binaries on eccentric orbits

Complete waveform model for compact binaries on eccentric orbits

Gravitational-wave phasing for low-eccentricity inspiralling compact binaries to 3PN order

Assessing the energetics of spinning binary black hole systems

Contact Info

Product

Resources

About